Remeis-Wiki - User contributions [en]

PhD Hat Dominic

2024-02-05T11:59:33Z

Sokolova-lapa:

[[Category:Internal]]
'''Info'''

'''Hat:'''

30x30cm platform (top), 15cm tube (base) Umfang: ??cm -> Steven

'''General:'''
*social media
*insta walk
*Bernreuther Dominic Social Media (BDSM) → Steven (''' to print''')
*tours and desperate wish to find a new guide planetarium half globe with clay planets → Aafia
*CCD -> print the most bulshit stuff written on the student report (?!)
*FRANCI (logo) → Steven (''' to print''')
*Christmass party (wok) → Ekaterina ('''DONE''')
*2bros and scam
*V2 rocket → Steven (''' to print''')
*car ford ka → knunchkugle (spherical car)
* Australia, Norway, fire etc. -> Australia Kangaroo upside down ('''DONE''')
*Australia -> map with "I can walk so far" ('''To print''')
* meeting Manami in the bakery → Ekaterina ('''DONE''')

'''science:'''

*training → lightbulbe -> Federico ('''DONE ''')
*Machine learning → pins colored representing layers of neural network connected with strings → Jonathan,Ole
*Bscan (actual Bee ) → Amy ('''DONE''')
*Bscam (Bubble Scanning Algorith [Module] Music) → Federico drive (not necessary)
*B - scam (scam emails) → Caro (/home/collischon/Documents/scammails.txt) -> ('''DONE''')
*bubble plastic with pictures of SNR → Jonathan ('''DONE''')
*soap bubbles as a tassle → Ole
*barcode scanner → Philipp
*blazar image (in the kitchen) → Steven (''' to print''')
* meme on the number of simulation -> Martin ('''DONE''')
* pool picture

'''Personal:'''
*Remeis coint (crypto currency) → Philipp
*?girlfriend has mushrooms he don't?
*mushroom picture, many mushrooms find the SNR (?)
*singing metal (tiny microphone) -> Federico ('''DONE''')
*or playing metal (mini instruments) →
*container houses -> globe with houses on top ('''DONE''')
*tiny houses around the word
*mountain bike
*motor bike (suzuki (susi)) mini models, probably 1st gen (1999—2002) SV650
*whiskey
*limoncello → paper bottle with bright yellow -> Katharina J. ('''DONE''')
*riesen (big riesen packed in another big riesen) (bunch of riesen that are found insted of the bubble) → Martin ('''DONE''')
*(horrible)chicken at the Rewe

[[Category:Internal]]

PhD Hat Dominic

2024-02-05T11:58:54Z

Sokolova-lapa:

[[Category:Internal]]
'''Info'''

'''Hat:'''

30x30cm platform (top), 15cm tube (base) Umfang: ??cm -> Steven

'''General:'''
*social media
*insta walk
*Bernreuther Dominic Social Media (BDSM) → Steven (''' to print''')
*tours and desperate wish to find a new guide planetarium half globe with clay planets → Aafia
*CCD -> print the most bulshit stuff written on the student report (?!)
*FRANCI (logo) → Steven (''' to print''')
*Christmass party (wok) → Ekaterina ('''DONE''')
*2bros and scam
*V2 rocket → Steven (''' to print''')
*car ford ka → knunchkugle (spherical car)
* Australia, Norway, fire etc. -> Australia Kangaroo upside down ('''DONE''')
*Australia -> map with "I can walk so far" ('''To print''')
* meeting Manami in the bakery → Ekaterina ('''To print''')

'''science:'''

*training → lightbulbe -> Federico ('''DONE ''')
*Machine learning → pins colored representing layers of neural network connected with strings → Jonathan,Ole
*Bscan (actual Bee ) → Amy ('''DONE''')
*Bscam (Bubble Scanning Algorith [Module] Music) → Federico drive (not necessary)
*B - scam (scam emails) → Caro (/home/collischon/Documents/scammails.txt) -> ('''DONE''')
*bubble plastic with pictures of SNR → Jonathan ('''DONE''')
*soap bubbles as a tassle → Ole
*barcode scanner → Philipp
*blazar image (in the kitchen) → Steven (''' to print''')
* meme on the number of simulation -> Martin ('''DONE''')
* pool picture

'''Personal:'''
*Remeis coint (crypto currency) → Philipp
*?girlfriend has mushrooms he don't?
*mushroom picture, many mushrooms find the SNR (?)
*singing metal (tiny microphone) -> Federico ('''DONE''')
*or playing metal (mini instruments) →
*container houses -> globe with houses on top ('''DONE''')
*tiny houses around the word
*mountain bike
*motor bike (suzuki (susi)) mini models, probably 1st gen (1999—2002) SV650
*whiskey
*limoncello → paper bottle with bright yellow -> Katharina J. ('''DONE''')
*riesen (big riesen packed in another big riesen) (bunch of riesen that are found insted of the bubble) → Martin ('''DONE''')
*(horrible)chicken at the Rewe

[[Category:Internal]]

PhD Hat Dominic

2024-01-31T10:37:44Z

Sokolova-lapa:

[[Category:Internal]]
'''Info'''

'''Hat:'''

30x30cm platform (top), 15cm tube (base) Umfang: ??cm -> Steven

'''General:'''
*social media
*insta walk
*Bernreuther Dominic Social Media (BDSM) → Steven
*tours and desperate wish to find a new guide planetarium half globe with clay planets → Aafia
*CCD -> print the most bulshit stuff written on the student report (?!)
*FRANCI (logo) → Steven
*Christmass party (wok) → Ekaterina
*2bros and scam
*V2 rocket → Steven
*car ford ka → knunchkugle (spherical car)
* Australia, Norway, fire etc. -> Australia Kangaroo upside down ('''DONE''')
* meeting Manami in the bakery → Ekaterina

'''science:'''

*training → lightbulbe -> Federico ('''DONE ''')
*Machine learning → pins colored representing layers of neural network connected with strings → Jonathan,Ole
*Bscan (actual Bee ) → Amy ('''DONE''')
*Bscam (Bubble Scanning Algorith [Module] Music) → Federico drive (not necessary)
*B - scam (scam emails) → Caro (/home/collischon/Documents/scammails.txt) -> ('''DONE''')
*bubble plastic with pictures of SNR → Jonathan ('''DONE''')
*soap bubbles as a tassle → Ole
*barcode scanner → Philipp
*blazar image (in the kitchen) → Steven
* meme on the number of simulation -> Martin ('''DONE''')

'''Personal:'''
*Remeis coint (crypto currency) → Philipp
*?girlfriend has mushrooms he don't?
*mushroom picture, many mushrooms find the SNR (?)
*singing metal (tiny microphone) -> Federico ('''DONE''')
*or playing metal (mini instruments) →
*container houses -> globe with houses on top ('''DONE''')
*tiny houses around the word
*mountain bike
*motor bike (suzuki (susi)) mini models, probably 1st gen (1999—2002) SV650
*whiskey
*limoncello → paper bottle with bright yellow -> Katharina J. ('''DONE''')
*riesen (big riesen packed in another big riesen) (bunch of riesen that are found insted of the bubble) → Martin ('''DONE''')
*(horrible)chicken at the Rewe

[[Category:Internal]]

Skivergnuegen 2024

2024-01-02T13:12:21Z

Sokolova-lapa: /* Aufteilung */

'''Remeis Skifahren 2024, 13.01.24-20.01.24''' The same procedure as every year ;-)
Hier werden die wichtigsten organisatorischen Dinge festgehalten. Jeder darf hier gerne editieren; wer keinen Account für das Wiki hat, muss sich bitte an jemanden wenden, der Zugang hat.

[[File:154854 silvretta-montafon-panorama.jpeg|right|700px]]

== Allgemeine Infos ==

*Ferienwohnung(en):
**Wir kommen wieder unter im [https://www.grandau.at/montafon/zimmer/ferienhaus-enzian Haus Enzian] des [https://www.grandau.at/ Sporthotels Grandau].
**Adresse des Sporthotel: Montafonerstraße 274a, 6791 St. Gallenkirch, Österreich. Unsere Unterkünfte liegen im Türkeiweg.

*Skigebiet: Montafon (Vorarlberg)
**Skigebiet Karte: https://winter.intermaps.com/montafon?lang=de
**Skipass Preise: https://www.silvretta-montafon.at/de/onlineshop/ticket-uebersicht
**Wer nicht alle 7 Tage Skifahren möchte: Es gibt Angebote wie z.B. 5 aus 6, mit einem solchen Skipass kann man innerhalb von 6 Tagen an 5 beliebigen Tagen skifahren.

*Skiverleih: [http://www.sportharry.at/ Sport Harry], direkt an der Talstation.

== Unterkunft ==
=== Aufteilung ===

Dieses Jahr gibt es die Hütte mit folgenden Zimmern (wir sind insgesamt 13-15, also bleiben keine Plätze frei).

{| class="wikitable"
! scope="col" | Zimmer
! scope="col" | Insassen
|-
! scope="row" | 2-er
|

|-
! scope="row" | 3-er
| Jakob, Katya
|-
! scope="row" | 4-er
| Eugenia (ab So, Einzelbett)
|-
! scope="row" | 5-er
|
|}

Außerdem gibt es ein Apartment für die Familien mit Kindern ;-): Eva+Steffen+Tom+Lorenz, Nela+Ohle+Sophia

== Fahrer ==
Fahrer können sich hier eintragen und Eckdaten angeben. Diejenige, die mitfahren möchten, sprechen sich mit den Fahrern ab und tragen sich ebenfalls ein. Klärt bitte auch die Gepäcklage, ggf. kann ein anderer Fahrer z.B. Skiausrüstung mitnehmen.

'''Auf der Suche nach einer Mitfahrgelegenheit: '''

{| class="wikitable"
! scope="col" | Fahrer
! scope="col" | # Plätze
! scope="col" | Anreise
! scope="col" | Mitfahrer Anreise
! scope="col" | Abreise
! scope="col" | Mitfahrer Abreise
! scope="col" | Skimitnahme
! scope="col" | Kommentar
|-
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|-
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|-
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|-

|-

|-

|-
|}

== Schwarzes Brett ==

=== Essen ===
Hier gibt's den Essensplan, soweit übernommen von den letzten Jahren. Da wir sehr viele Leute sind, sollten wir wieder vorab grob planen, was wir kochen wollen. Wir können einige Dinge in Deutschland besorgen und mitnehmen, es gib aber auch einen nahe gelegen Supermarkt. Generelle Dinge, wie z.B. Gewürze oder Aufstriche für Frühstücksbrötchen könnte man auch mitbringen.

Wer Kochvorschläge oder andere Ideen hat, gerne unten eintragen und kommentieren. Bedenkt, dass die Zubereitung (relativ) einfach sein sollte. Da sich die Liste in den letzten Jahren gut bewaehrt hat, behalten wir sie bei, aber die Reihenfolge/Tage kann man sicher noch hin und her bewegen. Einige (wenige) Sachen müssen wir dann manchmal trotzdem noch beim Spar kaufen, da ja auch der Kühlschrank nur begrenzt Platz hat.

'''Essenplan:'''
*Samstag: Spaghetti Bolognese + veg. Bolognese
*Sonntag: Käse Spätzle
*Montag: Burritos
*Dienstag: Risotto
*Mittwoch: Gulasch
*Donnerstag: Kartoffeln mit Kräuter-Quark
*Freitag: Dal mit Reis (od. Curry mit Suesskartoffeln )

Einkaufsliste von 2022 (vorletztes Jahr): https://docs.google.com/document/d/166b_mIXxmoAgcv1upIGremd_36E1fmwwxsQADP2uEv8/

@Christian: Vegane Option entwender selbst mitbringen oder hier mit reinschreiben (falls man die einfach bekommt)

=== Alkohol/Party ===

Stiegl (Johannes?)

=== Spiele ===

Immer lustig sind gemeinsame Spieleabende. Also, wer im Besitz von Gesellschaftsspielen ist, bringt diese gerne mit! Um eine Übersicht zu bekommen auch bitte hier eintragen:

''* Secret Hitler (Johannes?)''

=== Sonstiges ===

=== Alternativprogramm ===
* Rodeln (http://www.montafon.at/de/urlaubswelten/echte_naturliebhaber/rodeln)
* Schneeschuhwandern (http://www.montafon.at/schneeschuhwanderungen)
* Therme (http://www.montafon.at/schwimmen), z.B. http://www.aqua-dome.at/de (ca. 130km entfernt!)

[[Category:Internal]]

Litclub

2023-11-07T09:38:03Z

Sokolova-lapa: /* What is LitClub? */

== What is LitClub? ==

LitClub is a weekly meeting held at the Dr. Karl Remeis Observatory for all observatory members. The meeting consists of a presentation of a scientific, astrophysics-related paper chosen by a speaker, who was selected to give a talk for the current week and is followed by a general discussion. The goals of the meeting are the following:

* to improve communication and presentation skills for bachelor, master, and PhD students
* to provide a platform for free and casual discussion of scientific topics
* to learn more ;-)
* to bring all our groups together

LitClub takes place on Tuesdays at 11:30, in the conference room in the main observatory building.

LitClub is a mandatory activity for all observatory members. All students are on the list of presenters. All postdocs are expected to contribute to the discussion and to take over the presentation in case the speaker has to cancel last minute.

Please find below the general rules and commonly asked questions.

== Organization ==

Every week a person is chosen to present a paper.

'''How a person is chosen?'''

The selection of a presenter is done semi-randomly by Ingo, taking into account information about people's availability. At the beginning of the semester, a table is sent around where you can enter your availability on certain weeks (yes, all students are expected to be available a respectable amount of weeks per semester to make a presentation). If an observatory member provided no information in the table, the LitClub organizers assume that this person is available on any given day. The presenter is informed about the presentation a few days in advance.

'''How a presented paper is chosen?'''

A presenter chooses a paper from a list below, which contain the classical ("must-read") astrophysics-related papers, as well as some new advanced in the field. A different paper can be chosen, either from a peer-reviewed journal or the arxiv and which is related to space science (including, e.g., planetary science, instruments, methods, ...). In case you want to present something different, for example, to talk about your part or present research, please inform the organizers: [mailto:astro-literature@lists.fau.de astro-literature@lists.fau.de].

'''How presentation is done?'''
Presentation at the LitClub requires a few prepared slides with the most essential information, which helps to guide you (and your audience) through your talk. Any time-consuming design features are strongly discouraged: you are expected to quickly prepare simple slides with valuable content.

== Frequently Asked Questions ==

'''Is it really mandatory for all students?'''

Yes.

'''What if I cannot present when I am asked?'''

In this case, you have to find a person who could present instead of you on the date. At the same time, you are expected to give a presentation within the following weeks.

'''What are acceptable reasons to not present, when I was asked?'''

Lectures and examinations - confirmed by schedule or vacation and sickness - confirmed with your supervisor. In the case of one of these reasons, please see the previous question. If you got sick on the day of the presentation and there was no time to find a different speaker, you will be shifted to one of the following weeks and LitClub will be conducted by one (or a few) of the observatory postdocs.

'''I have an upcoming conference talk, is it a good reason to not present at LitClub a week before?'''

No. It is expected that the LitClub will not take too much of your preparation time. If it does - you need (want) to learn how to make it quicker, which is possible only by practice.

'''I am working on my master (bachelor/PhD) thesis, is it an acceptable reason to not present at LitClub?'''

No. Only if you have your defence within a few days of the LitClub in question. Otherwise: it is the time for you to work with a lot of literature. Just pick one of the papers you recently read for your thesis and present it.

'''Do I have to have slides for the presentation'''

Yes. The current request by our professors is that you would prepare simple slides with the main information. (5 slides is plenty)

'''How much time I am expected to spend to prepare for the LitClub presentation?'''

It depends on the paper you choose, but in general, you should be able to prepare your talk within half of a working day.

== Contact ==

For questions and comments, please contact the organizers: [mailto:astro-literature@lists.fau.de astro-literature@lists.fau.de].
Any major modifications to the structure of LitClub will be discussed with the professors.

== Litclub Paper List (WILL BE UPDATED!!!)==

We collect potentially interesting papers in an [https://ui.adsabs.harvard.edu/user/libraries/8mOwkXjvQl206110FBulVw ADS library] to give some inspiration (a separate [https://ui.adsabs.harvard.edu/user/libraries/9B-WkBVbTAmnzI7rmQ7dtA library] lists the already presented papers). But everyone is encouraged to present any interesting scientific work, not restricted to astronomy! Also, in case you found interesting papers feel free to add them to the list below (create sections as required).

=== X-ray astronomy ===

- Electromagnetic extraction of energy from Kerr black holes (Blandford-Znajek mechanism): Blandford, Znajek, MNRAS 179, 433, 1977 <ref>[https://ui.adsabs.harvard.edu/abs/1977MNRAS.179..433B/abstract]Blandford, Znajek, MNRAS 179, 433, 1977</ref> (although, astrophysically, the Blandford-Payne mechanism likely contributes more to jet launching, e.g., Livio, Ogilvie, Pringle, ApJ 512, 100, 1999)

- "The corona contracts in a black-hole transient": Kara et al., Nature 565 198, 2019 <ref>[https://ui.adsabs.harvard.edu/abs/2019Natur.565..198K/abstract]Kara et al., Nature 565 198, 2019</ref>, although this result is disputed (e.g., arxiv/2112.08116)

- Connection of FRBs and magnetars: "INTEGRAL Discovery of a Burst with Associated Radio Emission from the Magnetar SGR 1935+2154" (Mereghetti, 2020ApJ...898L..29M)

- "Discovery of oscillations above 200 keV in a black hole X-ray binary with Insight-HXMT" (Ma et al., 2021NatAs...5...94M)

- "Cygnus X-1 contains a 21-solar mass black hole—Implications for massive star winds" (Miller-Jones 2021Sci...371.1046M)

- EuCAPT White Paper: Opportunities and Challenges for Theoretical Astroparticle Physics in the Next Decade (Batista et al., arxiv.org/abs/2110.10074) - perhaps too long but really interesting summary

- Dark Energy Survey 3 Year Results (e.g., http://adsabs.harvard.edu/abs/2021arXiv210513549D)

=== Aliens? :0 ===

- Estimating the prevalence of malicious extraterrestrial civilizations (Caballero 2022arXiv220511618C) [https://arxiv.org/pdf/2205.11618.pdf]

=== Cosmology ===

- Is the Expansion of the Universe Accelerating? All Signs Still Point to Yes: A Local Dipole Anisotropy Cannot Explain Dark Energy [https://iopscience.iop.org/article/10.3847/1538-4357/ab7a16/pdf]

=== Statistics ===

- "STATISTICS, HANDLE WITH CARE: DETECTING MULTIPLE MODEL COMPONENTS WITH THE LIKELIHOOD RATIO TEST" (Protassov, 2002ApJ...571..545P)

=== Some more extravagant stuff ===

- The Breakthrough Listen Search For Intelligent Life Near the Galactic Center (Gajjar et al., ApJ 162, 33, 2021)

- An Objective Bayesian Analysis of Life's Early Start and Our Late Arrival (Kipping, 2020, https://arxiv.org/abs/2005.09008)

=== Non-astrophysics ===

- creating unique random numbers using the quantum noise of the vacuum: Gabriel et al., Nature Photonics 4, 711, 2010

Litclub

2023-10-24T15:27:48Z

Sokolova-lapa:

== What is LitClub? ==

LitClub is a weekly meeting held at the Dr. Karl Remeis Observatory for all observatory members. The meeting consists of a presentation of a scientific, astrophysics-related paper chosen by a speaker, who was selected to give a talk for the current week and is followed by a general discussion. The goals of the meeting are the following:

* to improve communication and presentation skills for bachelor, master, and PhD students
* to provide a platform for free and casual discussion of scientific topics
* to learn more ;-)
* to bring all our groups together

LitClub takes place on Tuesdays at 11:00, in the conference room in the main observatory building.

LitClub is a mandatory activity for all observatory members. All students are on the list of presenters. All postdocs are expected to contribute to the discussion and to take over the presentation in case the speaker has to cancel last minute.

Please find below the general rules and commonly asked questions.

== Organization ==

Every week a person chosen to present a paper.

'''How a person is chosen?'''

The selection of a presenter is done semi-randomly by Ingo, taking into account information about people's availability. At the beginning of the semester, a table is sent around where you can enter your availability on certain weeks (yes, all students are expected to be available a respectable amount of weeks per semester to make a presentation). If an observatory member provided no information in the table, the LitClub organizers assume that this person is available on any given day. A presenter is informed about the presentation a few days in advance.

'''How a presented paper is chosen?'''

A presenter chooses a paper from a list below, which contain the classical ("must-read") astrophysics-related papers, as well as some new advanced in the field. A different paper can be chosen, providing that it comes from a peer-reviewed journal and is clearly related to astrophysics (down to planetary science and instruments). In case you want to present something different, for example, to talk about your part or present research, please contact the organizers to agree on this case:
[mailto:astro-literature@lists.fau.de astro-literature@lists.fau.de].

'''How presentation is done?'''
Presentation at LitClub requires a few prepared slides with the most essential information, which helps guide you (and your audience) through your talk. Any time-consuming design features are strongly discouraged: as you are expected to prepare a plane and quick slides with valuable content.

== Frequently Asked Questions ==

'''Is it really mandatory for all students?'''

Yes.

'''What if I cannot present when I am asked?'''

In this case, you have to find a person who could present instead of you on the date. At the same time, you are expected to give a presentation within a few following weeks.

'''What is a respectful reason to not present, when I was asked?'''

Lectures and examinations - confirmed by schedule or vacation and sickness - confirmed with your supervisor. In the case of one of these reasons, please see a previous question. If you got sick on the day of the presentation and there was no time to find a different speaker, you will be shifted to one of the following weeks and LitClub will be conducted by one (or a few) of the observatory postdocs.

'''I have an upcoming conference talk, is it a good reason to not present at LitClub a week before?'''

No. It is expected that the LitClub will not take too much of your preparation time. If it does - you need (want) to learn how to make it quicker, which is possible only by practice.

'''I am working on my master (bachelor/PhD) thesis, is it a respectful reason to not present at LitClub?'''

No. Only if you have a defence within a few days of the LitClub in question. Otherwise: it is a really time for you to work with a lot of literature. Just pick one of the papers you read recently for your thesis and present it.

'''Do I have to have slides for the presentation'''

Yes. The current request by our professors is that you would prepare simple slides with the main information.

'''How much time I am expected to spend to prepare for the LitClub presentation?'''

It depends on the paper you choose, but in general, you should be able to prepare your talk within half of a working day.

== Contact ==

For questions and comments, please contact the organizers: [mailto:astro-literature@lists.fau.de astro-literature@lists.fau.de].
Any major modifications to the structure of LitClub will be discussed with the professors.

== Litclub Paper List (WILL BE UPDATED!!!)==

We collect potentially interesting papers in an [https://ui.adsabs.harvard.edu/user/libraries/8mOwkXjvQl206110FBulVw ADS library] to give some inspiration (a separate [https://ui.adsabs.harvard.edu/user/libraries/9B-WkBVbTAmnzI7rmQ7dtA library] lists the already presented papers). But everyone is encouraged to present any interesting scientific work, not restricted to astronomy! Also, in case you found interesting papers feel free to add them to the list below (create sections as required).

=== X-ray astronomy ===

- Electromagnetic extraction of energy from Kerr black holes (Blandford-Znajek mechanism): Blandford, Znajek, MNRAS 179, 433, 1977 <ref>[https://ui.adsabs.harvard.edu/abs/1977MNRAS.179..433B/abstract]Blandford, Znajek, MNRAS 179, 433, 1977</ref> (although, astrophysically, the Blandford-Payne mechanism likely contributes more to jet launching, e.g., Livio, Ogilvie, Pringle, ApJ 512, 100, 1999)

- "The corona contracts in a black-hole transient": Kara et al., Nature 565 198, 2019 <ref>[https://ui.adsabs.harvard.edu/abs/2019Natur.565..198K/abstract]Kara et al., Nature 565 198, 2019</ref>, although this result is disputed (e.g., arxiv/2112.08116)

- Connection of FRBs and magnetars: "INTEGRAL Discovery of a Burst with Associated Radio Emission from the Magnetar SGR 1935+2154" (Mereghetti, 2020ApJ...898L..29M)

- "Discovery of oscillations above 200 keV in a black hole X-ray binary with Insight-HXMT" (Ma et al., 2021NatAs...5...94M)

- "Cygnus X-1 contains a 21-solar mass black hole—Implications for massive star winds" (Miller-Jones 2021Sci...371.1046M)

- EuCAPT White Paper: Opportunities and Challenges for Theoretical Astroparticle Physics in the Next Decade (Batista et al., arxiv.org/abs/2110.10074) - perhaps too long but really interesting summary

- Dark Energy Survey 3 Year Results (e.g., http://adsabs.harvard.edu/abs/2021arXiv210513549D)

=== Aliens? :0 ===

- Estimating the prevalence of malicious extraterrestrial civilizations (Caballero 2022arXiv220511618C) [https://arxiv.org/pdf/2205.11618.pdf]

=== Cosmology ===

- Is the Expansion of the Universe Accelerating? All Signs Still Point to Yes: A Local Dipole Anisotropy Cannot Explain Dark Energy [https://iopscience.iop.org/article/10.3847/1538-4357/ab7a16/pdf]

=== Statistics ===

- "STATISTICS, HANDLE WITH CARE: DETECTING MULTIPLE MODEL COMPONENTS WITH THE LIKELIHOOD RATIO TEST" (Protassov, 2002ApJ...571..545P)

=== Some more extravagant stuff ===

- The Breakthrough Listen Search For Intelligent Life Near the Galactic Center (Gajjar et al., ApJ 162, 33, 2021)

- An Objective Bayesian Analysis of Life's Early Start and Our Late Arrival (Kipping, 2020, https://arxiv.org/abs/2005.09008)

=== Non-astrophysics ===

- creating unique random numbers using the quantum noise of the vacuum: Gabriel et al., Nature Photonics 4, 711, 2010

Phd hat list

2023-06-15T18:06:04Z

Sokolova-lapa:

{| class="wikitable"
! Name
! submission date
! defense date
! responsible person for the hat
|-
| Max L.
|
|
| Christian K.
|-
| Dominic
| 2023
|
|-
| Katya
| 2023
|
| Jakob
|-
| Christian K.
|
|
| Ole
|-
| Ole
|
|
| Philipp T.
|-
| Matti
| 2023
|
| Steven
|-
| Jakob
| 2023
|
| Katya
|-
| Max L.
| 202?
|
|
|-
|-
| Philipp T.
| 202?
|
|
|-
|-
| Caro
| 202?
|
|
|-
| Amy
| 202?
|
|
|-
| Steven
| 2024/2025???
|
|
|-
| Aafia
| 202?
|
|
|-
| Felix
| 202?
|
|
|-
| Federico
| 202?
|
|
|-
| Philipp W.
| 202?
|
|
|-
| Lea
| 202?
|
|
|-
| Mirjam
|
|
|
|-
| Eugenia
|
|
| Ralf
|-
|}

[[Category:Internal]]

Phd hat list

2023-06-15T18:05:45Z

Sokolova-lapa:

{| class="wikitable"
! Name
! submission date
! defense date
! responsible person for the hat
|-
| Max L.
|
|
| Christian K.
|-
| Dominic
| 2023
|
|-
| Katya
| 2023
|
| Jakob
|-
| Christian K.
|
|
| Ole
|-
| Ole
|
|
| Philipp T.
|-
| Matti
| 2023
|
| Steven
|-
| Jakob
| 2023
|
| Katya
|-
| Max L.
| 202?
|
|
|-
|-
| Philipp T.
| 202?
|
|
|-
|-
| Caro
| 202?
|
|
|-
| Amy
| 202?
|
|
|-
| Steven
| 2024/2025???
|
|
|-
| Aafia
| 202?
|
|
|-
| Felix
| 202?
|
|
|-
| Federico
| 202?
|
|
|-
| Philipp W.
| 202?
|
|
|-
| Lea
| 202?
|
|
|-
| Mirjam
|
| ?
|
|-
| Eugenia
|
|
| Ralf
|-
|}

[[Category:Internal]]

Phd hat list

2023-06-15T18:05:11Z

Sokolova-lapa:

{| class="wikitable"
! Name
! submission date
! defense date
! responsible person for the hat
|-
| Max L.
|
|
| Christian K.
|-
| Dominic
| 2023
|
|-
| Katya
| 2023
|
| Jakob
|-
| Christian K.
|
|
| Ole
|-
| Ole
|
|
| Philipp T.
|-
| Matti
| 2023
|
| Steven
|-
| Jakob
| 2023
|
| Katya
|-
| Max L.
| 202?
|
|
|-
|-
| Philipp T.
| 202?
|
|
|-
|-
| Caro
| 202?
|
|
|-
| Amy
| 202?
|
|
|-
| Steven
| 2024/2025???
|
|
|-
| Aafia
| 2024
|
|
|-
| Felix
| 2024
|
|
|-
| Federico
| 2024
|
|
|-
| Philipp W.
| 2024
|
|
|-
| Lea
| 2025
|
|
|-
| Mirjam
|
| ?
|
|-
| Eugenia
|
|
| Ralf
|-
|}

[[Category:Internal]]

Skivergnuegen 2023

2023-01-03T16:00:16Z

Sokolova-lapa: /* Fahrer */

'''Remeis Skifahren 2023''' The same procedure as every year ;-)
Hier werden die wichtigsten organisatorischen Dinge festgehalten. Jeder darf hier gerne editieren; wer keinen Account für das Wiki hat, muss sich bitte an jemanden wenden, der Zugang hat.

[[File:154854 silvretta-montafon-panorama.jpeg|right|700px]]

== Allgemeine Infos ==

*Ferienwohnung(en):
**Wir kommen wieder unter im [https://www.grandau.at/montafon/zimmer/ferienhaus-enzian Haus Enzian] des [https://www.grandau.at/ Sporthotels Grandau].
**Adresse des Sporthotel: Montafonerstraße 274a, 6791 St. Gallenkirch, Österreich. Unsere Unterkünfte liegen im Türkeiweg.

*Skigebiet: Montafon (Vorarlberg)
**Skigebiet Karte: https://winter.intermaps.com/montafon?lang=de
**Skipass Preise: https://www.montafon.at/de/Service/Bergbahn-Preise-Tickets/Mehrtageskarte-Winter
**Wer nicht alle 7 Tage Skifahren möchte: Es gibt Angebote wie z.B. 5 aus 7, mit einem solchen Skipass kann man innerhalb von 7 Tagen an 5 beliebigen Tagen skifahren.

*Skiverleih: [http://www.sportharry.at/ Sport Harry], direkt an der Talstation.

== Unterkunft ==
=== Aufteilung ===

Dieses Jahr gibt es nur die Hütte mit folgenden Zimmern (wir sind insgesamt 14, also bleiben keine Plätze frei).

{| class="wikitable"
! scope="col" | Zimmer
! scope="col" | Insassen
|-
! scope="row" | 2-er
| Amy, Aafia

|-
! scope="row" | 3-er
| Jakob, Max, Katya
|-
! scope="row" | 4-er
| Eva, Steffen, Flo, Christian
|-
! scope="row" | 5-er
| Basti, Philipp
|}

== Fahrer ==
Fahrer können sich hier eintragen und Eckdaten angeben. Diejenige, die mitfahren möchten, sprechen sich mit den Fahrern ab und tragen sich ebenfalls ein. Klärt bitte auch die Gepäcklage, ggf. kann ein anderer Fahrer z.B. Skiausrüstung mitnehmen.

'''Auf der Suche nach einer Mitfahrgelegenheit: '''

{| class="wikitable"
! scope="col" | Fahrer
! scope="col" | # Plätze
! scope="col" | Anreise
! scope="col" | Mitfahrer Anreise
! scope="col" | Abreise
! scope="col" | Mitfahrer Abreise
! scope="col" | Skimitnahme
! scope="col" | Kommentar
|-
|Eva
|0(3)
|Samstag
|Steffen+Christian
|Samstag?
|Steffen+Christian
|eigene ja
|Auto ist voll
|-
|Max
|0(3)
|Samstag (from Arlberg)
|Jakob+Katya
|Samstag
|Jakob+Katya
|eigene ja
|Auto ist voll
|-
|Basti
|3(3)
|Sonntag ganz frueh
|
|Freitag Mittag
|
|Ja
|
|-

|-

|-

|-
|}

== Schwarzes Brett ==

=== Essen ===
Hier gibt's den Essensplan, soweit übernommen von den letzten Jahren. Da wir sehr viele Leute sind, sollten wir wieder vorab grob planen, was wir kochen wollen. Wir können einige Dinge in Deutschland besorgen und mitnehmen, es gib aber auch einen nahe gelegen Supermarkt. Generelle Dinge, wie z.B. Gewürze oder Aufstriche für Frühstücksbrötchen könnte man auch mitbringen.

Wer Kochvorschläge oder andere Ideen hat, gerne unten eintragen und kommentieren. Bedenkt, dass die Zubereitung (relativ) einfach sein sollte. Da sich die Liste in den letzten Jahren gut bewaehrt hat, behalten wir sie bei, aber die Reihenfolge/Tage kann man sicher noch hin und her bewegen. Einige (wenige) Sachen müssen wir dann manchmal trotzdem noch beim Spar kaufen, da ja auch der Kühlschrank nur begrenzt Platz hat.

'''Essenplan:'''
*Samstag: Spaghetti Bolognese + veg. Bolognese
*Sonntag: Käse Spätzle
*Montag: Burritos
*Dienstag: Risotto
*Mittwoch: Gulasch
*Donnerstag: Kartoffeln mit Kräuter-Quark
*Freitag: Dal mit Reis (od. Curry mit Suesskartoffeln )

Einkaufsliste von 2022 (letztes Jahr): https://docs.google.com/document/d/166b_mIXxmoAgcv1upIGremd_36E1fmwwxsQADP2uEv8/

@Christian: Vegane Option entwender selbst mitbringen oder hier mit reinschreiben (falls man die einfach bekommt)

=== Alkohol/Party ===

=== Spiele ===

Immer lustig sind gemeinsame Spieleabende. Also, wer im Besitz von Gesellschaftsspielen ist, bringt diese gerne mit! Um eine Übersicht zu bekommen auch bitte hier eintragen:

''* Spiele hier eintragen''

=== Sonstiges ===

=== Alternativprogramm ===
* Rodeln (http://www.montafon.at/de/urlaubswelten/echte_naturliebhaber/rodeln)
* Schneeschuhwandern (http://www.montafon.at/schneeschuhwanderungen)
* Therme (http://www.montafon.at/schwimmen), z.B. http://www.aqua-dome.at/de (ca. 130km entfernt!)

[[Category:Internal]]

Skivergnuegen 2023

2022-12-30T15:33:01Z

Sokolova-lapa: /* Aufteilung */

'''Remeis Skifahren 2023''' The same procedure as every year ;-)
Hier werden die wichtigsten organisatorischen Dinge festgehalten. Jeder darf hier gerne editieren; wer keinen Account für das Wiki hat, muss sich bitte an jemanden wenden, der Zugang hat.

[[File:154854 silvretta-montafon-panorama.jpeg|right|700px]]

== Allgemeine Infos ==

*Ferienwohnung(en):
**Wir kommen wieder unter im [https://www.grandau.at/montafon/zimmer/ferienhaus-enzian Haus Enzian] des [https://www.grandau.at/ Sporthotels Grandau].
**Adresse des Sporthotel: Montafonerstraße 274a, 6791 St. Gallenkirch, Österreich. Unsere Unterkünfte liegen im Türkeiweg.

*Skigebiet: Montafon (Vorarlberg)
**Skigebiet Karte: https://winter.intermaps.com/montafon?lang=de
**Skipass Preise: https://www.montafon.at/de/Service/Bergbahn-Preise-Tickets/Mehrtageskarte-Winter
**Wer nicht alle 7 Tage Skifahren möchte: Es gibt Angebote wie z.B. 5 aus 7, mit einem solchen Skipass kann man innerhalb von 7 Tagen an 5 beliebigen Tagen skifahren.

*Skiverleih: [http://www.sportharry.at/ Sport Harry], direkt an der Talstation.

== Unterkunft ==
=== Aufteilung ===

Dieses Jahr gibt es nur die Hütte mit folgenden Zimmern (wir sind insgesamt 14, also bleiben keine Plätze frei).

{| class="wikitable"
! scope="col" | Zimmer
! scope="col" | Insassen
|-
! scope="row" | 2-er
| Amy, Aafia

|-
! scope="row" | 3-er
| Jakob, Max, Katya
|-
! scope="row" | 4-er
| Eva, Steffen, Flo, Christian
|-
! scope="row" | 5-er
|
|}

== Fahrer ==
Fahrer können sich hier eintragen und Eckdaten angeben. Diejenige, die mitfahren möchten, sprechen sich mit den Fahrern ab und tragen sich ebenfalls ein. Klärt bitte auch die Gepäcklage, ggf. kann ein anderer Fahrer z.B. Skiausrüstung mitnehmen.

'''Auf der Suche nach einer Mitfahrgelegenheit: '''

{| class="wikitable"
! scope="col" | Fahrer
! scope="col" | # Plätze
! scope="col" | Anreise
! scope="col" | Mitfahrer Anreise
! scope="col" | Abreise
! scope="col" | Mitfahrer Abreise
! scope="col" | Skimitnahme
! scope="col" | Kommentar
|-
|Eva
|0(3)
|Samstag
|Steffen+Christian
|Samstag?
|Steffen+Christian
|eigene ja
|Auto ist voll
|-

|-

|-

|-

|-
|}

== Schwarzes Brett ==

=== Essen ===
Hier gibt's den Essensplan, soweit übernommen von den letzten Jahren. Da wir sehr viele Leute sind, sollten wir wieder vorab grob planen, was wir kochen wollen. Wir können einige Dinge in Deutschland besorgen und mitnehmen, es gib aber auch einen nahe gelegen Supermarkt. Generelle Dinge, wie z.B. Gewürze oder Aufstriche für Frühstücksbrötchen könnte man auch mitbringen.

Wer Kochvorschläge oder andere Ideen hat, gerne unten eintragen und kommentieren. Bedenkt, dass die Zubereitung (relativ) einfach sein sollte. Da sich die Liste in den letzten Jahren gut bewaehrt hat, behalten wir sie bei, aber die Reihenfolge/Tage kann man sicher noch hin und her bewegen. Einige (wenige) Sachen müssen wir dann manchmal trotzdem noch beim Spar kaufen, da ja auch der Kühlschrank nur begrenzt Platz hat.

'''Essenplan:'''
*Samstag: Spaghetti Bolognese + veg. Bolognese
*Sonntag: Käse Spätzle
*Montag: Burritos
*Dienstag: Risotto
*Mittwoch: Gulasch
*Donnerstag: Kartoffeln mit Kräuter-Quark
*Freitag: Dal mit Reis (od. Curry mit Suesskartoffeln )

Einkaufsliste von 2022 (letztes Jahr): https://docs.google.com/document/d/166b_mIXxmoAgcv1upIGremd_36E1fmwwxsQADP2uEv8/

@Christian: Vegane Option entwender selbst mitbringen oder hier mit reinschreiben (falls man die einfach bekommt)

=== Alkohol/Party ===

=== Spiele ===

Immer lustig sind gemeinsame Spieleabende. Also, wer im Besitz von Gesellschaftsspielen ist, bringt diese gerne mit! Um eine Übersicht zu bekommen auch bitte hier eintragen:

''* Spiele hier eintragen''

=== Sonstiges ===

=== Alternativprogramm ===
* Rodeln (http://www.montafon.at/de/urlaubswelten/echte_naturliebhaber/rodeln)
* Schneeschuhwandern (http://www.montafon.at/schneeschuhwanderungen)
* Therme (http://www.montafon.at/schwimmen), z.B. http://www.aqua-dome.at/de (ca. 130km entfernt!)

[[Category:Internal]]

Skivergnuegen 2023

2022-12-30T13:41:40Z

Sokolova-lapa: /* Aufteilung */

'''Remeis Skifahren 2023''' The same procedure as every year ;-)
Hier werden die wichtigsten organisatorischen Dinge festgehalten. Jeder darf hier gerne editieren; wer keinen Account für das Wiki hat, muss sich bitte an jemanden wenden, der Zugang hat.

[[File:154854 silvretta-montafon-panorama.jpeg|right|700px]]

== Allgemeine Infos ==

*Ferienwohnung(en):
**Wir kommen wieder unter im [https://www.grandau.at/montafon/zimmer/ferienhaus-enzian Haus Enzian] des [https://www.grandau.at/ Sporthotels Grandau].
**Adresse des Sporthotel: Montafonerstraße 274a, 6791 St. Gallenkirch, Österreich. Unsere Unterkünfte liegen im Türkeiweg.

*Skigebiet: Montafon (Vorarlberg)
**Skigebiet Karte: https://winter.intermaps.com/montafon?lang=de
**Skipass Preise: https://www.montafon.at/de/Service/Bergbahn-Preise-Tickets/Mehrtageskarte-Winter
**Wer nicht alle 7 Tage Skifahren möchte: Es gibt Angebote wie z.B. 5 aus 7, mit einem solchen Skipass kann man innerhalb von 7 Tagen an 5 beliebigen Tagen skifahren.

*Skiverleih: [http://www.sportharry.at/ Sport Harry], direkt an der Talstation.

== Unterkunft ==
=== Aufteilung ===

Dieses Jahr gibt es nur die Hütte mit folgenden Zimmern (wir sind insgesamt 14, also bleiben keine Plätze frei).

{| class="wikitable"
! scope="col" | Zimmer
! scope="col" | Insassen
|-
! scope="row" | 2-er
| Amy, Aafia

|-
! scope="row" | 3-er
| Jakob, Katya, Max (?)
|-
! scope="row" | 4-er
| Eva, Steffen, Flo, Christian
|-
! scope="row" | 5-er
|
|}

== Fahrer ==
Fahrer können sich hier eintragen und Eckdaten angeben. Diejenige, die mitfahren möchten, sprechen sich mit den Fahrern ab und tragen sich ebenfalls ein. Klärt bitte auch die Gepäcklage, ggf. kann ein anderer Fahrer z.B. Skiausrüstung mitnehmen.

'''Auf der Suche nach einer Mitfahrgelegenheit: '''

{| class="wikitable"
! scope="col" | Fahrer
! scope="col" | # Plätze
! scope="col" | Anreise
! scope="col" | Mitfahrer Anreise
! scope="col" | Abreise
! scope="col" | Mitfahrer Abreise
! scope="col" | Skimitnahme
! scope="col" | Kommentar
|-
|Eva
|0(3)
|Samstag
|Steffen+Christian
|Samstag?
|Steffen+Christian
|eigene ja
|Auto ist voll
|-

|-

|-

|-

|-
|}

== Schwarzes Brett ==

=== Essen ===
Hier gibt's den Essensplan, soweit übernommen von den letzten Jahren. Da wir sehr viele Leute sind, sollten wir wieder vorab grob planen, was wir kochen wollen. Wir können einige Dinge in Deutschland besorgen und mitnehmen, es gib aber auch einen nahe gelegen Supermarkt. Generelle Dinge, wie z.B. Gewürze oder Aufstriche für Frühstücksbrötchen könnte man auch mitbringen.

Wer Kochvorschläge oder andere Ideen hat, gerne unten eintragen und kommentieren. Bedenkt, dass die Zubereitung (relativ) einfach sein sollte. Da sich die Liste in den letzten Jahren gut bewaehrt hat, behalten wir sie bei, aber die Reihenfolge/Tage kann man sicher noch hin und her bewegen. Einige (wenige) Sachen müssen wir dann manchmal trotzdem noch beim Spar kaufen, da ja auch der Kühlschrank nur begrenzt Platz hat.

'''Essenplan:'''
*Samstag: Spaghetti Bolognese + veg. Bolognese
*Sonntag: Käse Spätzle
*Montag: Burritos
*Dienstag: Risotto
*Mittwoch: Gulasch
*Donnerstag: Kartoffeln mit Kräuter-Quark
*Freitag: Dal mit Reis (od. Curry mit Suesskartoffeln )

Einkaufsliste von 2022 (letztes Jahr): https://docs.google.com/document/d/166b_mIXxmoAgcv1upIGremd_36E1fmwwxsQADP2uEv8/

@Christian: Vegane Option entwender selbst mitbringen oder hier mit reinschreiben (falls man die einfach bekommt)

=== Alkohol/Party ===

=== Spiele ===

Immer lustig sind gemeinsame Spieleabende. Also, wer im Besitz von Gesellschaftsspielen ist, bringt diese gerne mit! Um eine Übersicht zu bekommen auch bitte hier eintragen:

''* Spiele hier eintragen''

=== Sonstiges ===

=== Alternativprogramm ===
* Rodeln (http://www.montafon.at/de/urlaubswelten/echte_naturliebhaber/rodeln)
* Schneeschuhwandern (http://www.montafon.at/schneeschuhwanderungen)
* Therme (http://www.montafon.at/schwimmen), z.B. http://www.aqua-dome.at/de (ca. 130km entfernt!)

[[Category:Internal]]

List of cyclotron line sources

2022-07-04T18:01:37Z

Sokolova-lapa:

[[Category:Accreting X-ray Pulsars]]

This table attempts to summarize all known cyclotron line sources. It is based on the presentation [http://astrons.sabanciuniv.edu/astrons2010/wordpress/wp-content/uploads/2009/12/Spectral-continua-of-accreting-neutron-star-systems.pdf "Spectral continua of accreting neutron star systems"] by Jörn Wilms at the conference
[http://astrons.sabanciuniv.edu/astrons2010/wordpress/ Astrophysics of Neutron Stars 2010] with some information added later.

T/P = Transient/Persistent

{| class="wikitable"
! #
! Source
! Ecyc [keV]
! Pspin [s]
! Porbital [d]
! Companion
! T/P
! Discovery
! Other ref
|-
|1
| [[Swift J1626.6-5156]]
|4.9, 8.4, 12.6, 16.9 <ref name="Molkov2021" />
| 15.4
| 132.9
|Be
|P
|Swift/BAT <ref name="Palmer2005" />
|<ref name="DeCesar09" />, <ref name="DeCesar2013" />
|-
| [[4U 0115+634]]
|14, 24, 36, 48, 62
| 3.6
| 24.3
|Be
|T
|HEAO-1 <ref name="Wheaton79" /> RXTE <ref name="Heindl99" />, BeppoSAX <ref name="Santangelo99" />
|-
| [[4U 1907+09]]
|18, 38
| 441
| 8.37
|B2 III-IV
|P
|BeppoSAX <ref name="Cusumano98b" />
|-
| [[4U 1538-52]]
|22, 47
| 530
| 3.7
|B0I
|P
|Ginga <ref name="Clark90" />, RXTE <ref name="RodesRoca09" />
|-
| [[Vela X-1]]
|24, 52
| 283
| 8.96
|B0.5Ib
|P
|Mir-HEXE <ref name="Kendziorra92" />, RXTE <ref name="Kreykenbohm02" />
|-
| [[V 0332+53]]
|27, 51, 74
| 4.37
| 34.25
|Be
|T
|Ginga <ref name="Makishima90" />
|-
| [[Cep X-4]]
|28
| 66.25
| >23
|B1
|T
|Ginga <ref name="Mihara91" />
|-
| [[Cen X-3]]
|29
| 4.8
| 2.09
|O6.5II
|P
|BeppoSAX <ref name="Santangelo98" />, RXTE <ref name="HeindlChakrabarty99" />
|-
| [[X Per]]
|29?
| 837
| 250.3
|B0 III–Ve
|P
|RXTE <ref name="Coburn01" />
|-
| [[RX J0440.9+4431]]
|32
| 203
| 155
|B0.2 Ve
|T
|INTEGRAL, RXTE + Swift <ref name="Tsygankov12" />
|-
| [[MXB 0656-072]]
|33
| 160
| 100?
|O9.7Ve
|T
|RXTE <ref name="Heindl03b" />
|-
| [[XTE J1946+274]]
|36
| 15.8
| 169.2
|B0-1V-IVe
|T
|RXTE <ref name="Heindl01" />
|-
| [[4U 1626-67]]
|37
| 7.66
| 0.028
|WD?
|P
|BeppoSAX <ref name="Orlandini98b" />, RXTE <ref name="HeindlChakrabarty99" />
|-
| [[GX 301-2]]
|37
| 690
| 41.5
|B1.2Ia
|P
|Ginga <ref name="MiharaPhD" />
|-
| [[Her X-1]]
|41
| 1.24
| 1.7
|A9-B
|P
|Ballon-HEXE <ref name="Truemper78" />
|-
| [[A0535+26]]
|45, 100+
| 104
| 110.6
|Be
|T
|HEXE <ref name="Kendziorra92" /><ref name="Kendziorra94" />, CGRO <ref name="Maisack97" />
|-
| [[1A1118-616]]
|55, 110?
| 408
| 400-800?
|O9.5IV-Ve
|T
|RXTE <ref name="Doroshenko10" />, Suzaku <ref name="Suchy11" />
|-
| [[GRO J1008-57]]
|88?
| 93.7
| 249.46
|B1-B2
|T
|CGRO <ref name="Shrader99" />
|-
| [[GX 304-1]]
|54
| 272
| 132.2
|B2 Vne
|P
|RXTE <ref name="Yamamoto11" />, INTEGRAL <ref name="Klochkov12" />
|-
| [[KS 1947+300]]
|12
| 18.8
| 40.4
|B0Ve
|T
|NuSTAR <ref name="Fuerst14a" />
|}

= Location in the Galaxy =

The figure below displays the position of the sources listed above in the Galaxy as far as known at this moment. Click on the figure for a larger version. Labels indicate the ordinal number in the first column of the table. Uncertainties in the distances are not indicated. Empty symbols represent sources for which there is no distance info in the literature; they have been artificially set to a distance
of 7.6 kpc. The spiral arms are from <ref name="Vallee08" />. Figure and data provided by Arash Bodaghee, SSL, UC Berkeley.

{| class="wikitable"
!
! #
! Source
! Dist. [kpc]
! Reference
|-
|rowspan="17"|[[File:cyclotronlinesourcesinthegalaxy.png|464px]]
| 1
| [[Swift J1626.6-5156]]
| 8±2.4
| <ref name="Reig11b" />
|-
| 2
| [[4U 0115+634]]
| 8±1
| <ref name="Negueruela01" />
|-
| 3
| [[4U 1907+09]]
| 5
| <ref name="Cox05" />
|-
| 4
| [[4U 1538-52]]
| 6.4±1
| <ref name="Reynolds92" />
|-
| 5
| [[Vela X-1]]
|1.4±0.5
| <ref name="ChevalierIlovaisky98" />
|-
| 6
| [[V 0332+53]]
|7.5±1.5
| <ref name="Negueruela99" />
|-
| 7
| [[Cep X-4]]
|3.8±0.6
| <ref name="BonnetBidaudMouchet98" />
|-
| 8
| [[Cen X-3]]
|10±1
| <ref name="Hutchings79" />
|-
| 9
| [[X Per]]
|0.7±0.3
| <ref name="Lyubimkov97" />
|-
| 10
| [[MXB 0656-072]]
|3.9±0.1
| <ref name="McBride06" />
|-
| 11
| [[XTE J1946+274]]
|9.5±2.9
| <ref name="Wilson03" />
|-
| 12
| [[4U 1626-67]]
|9
| <ref name="GrimmGilfanovSunyaev02" />
|-
| 13
| [[GX 301-2]]
|4.1
| <ref name="Leahy02a" />
|-
| 14
| [[Her X-1]]
|6.6±0.4
| <ref name="Reynolds97" />
|-
| 15
| [[A0535+26]]
|2-0.7+0.4
| <ref name="Steele98" />
|-
| 16
| [[1A1118−61]]
|5±2
| <ref name="JanotPacheco81" />
|-
| 17
| [[xrp:gro_j1008-57|GRO J1008−57]]
|5
| <ref name="GrimmGilfanovSunyaev02" />
|}

= References =

List of cyclotron line sources

2022-07-04T18:00:52Z

Sokolova-lapa:

[[Category:Accreting X-ray Pulsars]]

This table attempts to summarize all known cyclotron line sources. It is based on the presentation [http://astrons.sabanciuniv.edu/astrons2010/wordpress/wp-content/uploads/2009/12/Spectral-continua-of-accreting-neutron-star-systems.pdf "Spectral continua of accreting neutron star systems"] by Jörn Wilms at the conference
[http://astrons.sabanciuniv.edu/astrons2010/wordpress/ Astrophysics of Neutron Stars 2010] with some information added later.

T/P = Transient/Persistent

{| class="wikitable"
! #
! Source
! Ecyc [keV]
! Pspin [s]
! Porbital [d]
! Companion
! T/P
! Discovery
! Other ref
|-
|1
| [[Swift J1626.6-5156]]
|4.9, 8.4, 12.6, 16.9 <ref name="Molkov2021" />
| 15.4
| 132.9
|Be
|P
|Swift/BAT <ref name="Palmer2005" />
|<ref name="DeCesar09" />, <ref name="DeCesar13" />
|-
| [[4U 0115+634]]
|14, 24, 36, 48, 62
| 3.6
| 24.3
|Be
|T
|HEAO-1 <ref name="Wheaton79" /> RXTE <ref name="Heindl99" />, BeppoSAX <ref name="Santangelo99" />
|-
| [[4U 1907+09]]
|18, 38
| 441
| 8.37
|B2 III-IV
|P
|BeppoSAX <ref name="Cusumano98b" />
|-
| [[4U 1538-52]]
|22, 47
| 530
| 3.7
|B0I
|P
|Ginga <ref name="Clark90" />, RXTE <ref name="RodesRoca09" />
|-
| [[Vela X-1]]
|24, 52
| 283
| 8.96
|B0.5Ib
|P
|Mir-HEXE <ref name="Kendziorra92" />, RXTE <ref name="Kreykenbohm02" />
|-
| [[V 0332+53]]
|27, 51, 74
| 4.37
| 34.25
|Be
|T
|Ginga <ref name="Makishima90" />
|-
| [[Cep X-4]]
|28
| 66.25
| >23
|B1
|T
|Ginga <ref name="Mihara91" />
|-
| [[Cen X-3]]
|29
| 4.8
| 2.09
|O6.5II
|P
|BeppoSAX <ref name="Santangelo98" />, RXTE <ref name="HeindlChakrabarty99" />
|-
| [[X Per]]
|29?
| 837
| 250.3
|B0 III–Ve
|P
|RXTE <ref name="Coburn01" />
|-
| [[RX J0440.9+4431]]
|32
| 203
| 155
|B0.2 Ve
|T
|INTEGRAL, RXTE + Swift <ref name="Tsygankov12" />
|-
| [[MXB 0656-072]]
|33
| 160
| 100?
|O9.7Ve
|T
|RXTE <ref name="Heindl03b" />
|-
| [[XTE J1946+274]]
|36
| 15.8
| 169.2
|B0-1V-IVe
|T
|RXTE <ref name="Heindl01" />
|-
| [[4U 1626-67]]
|37
| 7.66
| 0.028
|WD?
|P
|BeppoSAX <ref name="Orlandini98b" />, RXTE <ref name="HeindlChakrabarty99" />
|-
| [[GX 301-2]]
|37
| 690
| 41.5
|B1.2Ia
|P
|Ginga <ref name="MiharaPhD" />
|-
| [[Her X-1]]
|41
| 1.24
| 1.7
|A9-B
|P
|Ballon-HEXE <ref name="Truemper78" />
|-
| [[A0535+26]]
|45, 100+
| 104
| 110.6
|Be
|T
|HEXE <ref name="Kendziorra92" /><ref name="Kendziorra94" />, CGRO <ref name="Maisack97" />
|-
| [[1A1118-616]]
|55, 110?
| 408
| 400-800?
|O9.5IV-Ve
|T
|RXTE <ref name="Doroshenko10" />, Suzaku <ref name="Suchy11" />
|-
| [[GRO J1008-57]]
|88?
| 93.7
| 249.46
|B1-B2
|T
|CGRO <ref name="Shrader99" />
|-
| [[GX 304-1]]
|54
| 272
| 132.2
|B2 Vne
|P
|RXTE <ref name="Yamamoto11" />, INTEGRAL <ref name="Klochkov12" />
|-
| [[KS 1947+300]]
|12
| 18.8
| 40.4
|B0Ve
|T
|NuSTAR <ref name="Fuerst14a" />
|}

= Location in the Galaxy =

The figure below displays the position of the sources listed above in the Galaxy as far as known at this moment. Click on the figure for a larger version. Labels indicate the ordinal number in the first column of the table. Uncertainties in the distances are not indicated. Empty symbols represent sources for which there is no distance info in the literature; they have been artificially set to a distance
of 7.6 kpc. The spiral arms are from <ref name="Vallee08" />. Figure and data provided by Arash Bodaghee, SSL, UC Berkeley.

{| class="wikitable"
!
! #
! Source
! Dist. [kpc]
! Reference
|-
|rowspan="17"|[[File:cyclotronlinesourcesinthegalaxy.png|464px]]
| 1
| [[Swift J1626.6-5156]]
| 8±2.4
| <ref name="Reig11b" />
|-
| 2
| [[4U 0115+634]]
| 8±1
| <ref name="Negueruela01" />
|-
| 3
| [[4U 1907+09]]
| 5
| <ref name="Cox05" />
|-
| 4
| [[4U 1538-52]]
| 6.4±1
| <ref name="Reynolds92" />
|-
| 5
| [[Vela X-1]]
|1.4±0.5
| <ref name="ChevalierIlovaisky98" />
|-
| 6
| [[V 0332+53]]
|7.5±1.5
| <ref name="Negueruela99" />
|-
| 7
| [[Cep X-4]]
|3.8±0.6
| <ref name="BonnetBidaudMouchet98" />
|-
| 8
| [[Cen X-3]]
|10±1
| <ref name="Hutchings79" />
|-
| 9
| [[X Per]]
|0.7±0.3
| <ref name="Lyubimkov97" />
|-
| 10
| [[MXB 0656-072]]
|3.9±0.1
| <ref name="McBride06" />
|-
| 11
| [[XTE J1946+274]]
|9.5±2.9
| <ref name="Wilson03" />
|-
| 12
| [[4U 1626-67]]
|9
| <ref name="GrimmGilfanovSunyaev02" />
|-
| 13
| [[GX 301-2]]
|4.1
| <ref name="Leahy02a" />
|-
| 14
| [[Her X-1]]
|6.6±0.4
| <ref name="Reynolds97" />
|-
| 15
| [[A0535+26]]
|2-0.7+0.4
| <ref name="Steele98" />
|-
| 16
| [[1A1118−61]]
|5±2
| <ref name="JanotPacheco81" />
|-
| 17
| [[xrp:gro_j1008-57|GRO J1008−57]]
|5
| <ref name="GrimmGilfanovSunyaev02" />
|}

= References =

List of references

2022-07-04T18:00:31Z

Sokolova-lapa: /* The library */

This page is used as a library for references.

== Using references on a page ==

In order to include references from this library in any page, simply add a <nowiki><ref name="..." /></nowiki> markup to the page's text at the corresponding position, e.g.,
<nowiki><ref name="Wilms2000a" /></nowiki>

== Adding references to the library ==

Adding a reference to the library here requires to define of a <nowiki><libref name="...">...</libref></nowiki> markup in the '''The library''' subsection below. The ''name'' attribute of the <nowiki><libref></nowiki>-tag identifies this reference, which can then be used on any page. The example above would be defined like this:
<nowiki><libref name="Wilms2000a"></nowiki>
<nowiki>Wilms, Allen, & McCray, 2000, ApJ 542, 914 ([http://adsabs.harvard.edu/abs/2000ApJ...542..914W NASA ADS])</nowiki>
<nowiki></libref></nowiki>
The text inside the <nowiki><libref></nowiki> markup gets pasted into the reference section of the page. Thus, please follow the [[The Remeis English Checklist#Citations|citation guidelines]] here! It is recommended to add a link to, e.g., the NASA ADS record as well.

== The library ==

This is the actual definition of the library. Add references here by editing this section.

<reflibrary>

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List of references

2022-07-04T16:54:43Z

Sokolova-lapa:

This page is used as a library for references.

== Using references on a page ==

In order to include references from this library in any page, simply add a <nowiki><ref name="..." /></nowiki> markup to the page's text at the corresponding position, e.g.,
<nowiki><ref name="Wilms2000a" /></nowiki>

== Adding references to the library ==

Adding a reference to the library here requires to define of a <nowiki><libref name="...">...</libref></nowiki> markup in the '''The library''' subsection below. The ''name'' attribute of the <nowiki><libref></nowiki>-tag identifies this reference, which can then be used on any page. The example above would be defined like this:
<nowiki><libref name="Wilms2000a"></nowiki>
<nowiki>Wilms, Allen, & McCray, 2000, ApJ 542, 914 ([http://adsabs.harvard.edu/abs/2000ApJ...542..914W NASA ADS])</nowiki>
<nowiki></libref></nowiki>
The text inside the <nowiki><libref></nowiki> markup gets pasted into the reference section of the page. Thus, please follow the [[The Remeis English Checklist#Citations|citation guidelines]] here! It is recommended to add a link to, e.g., the NASA ADS record as well.

== The library ==

This is the actual definition of the library. Add references here by editing this section.

<reflibrary>

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List of cyclotron line sources

2022-07-04T16:27:12Z

Sokolova-lapa:

[[Category:Accreting X-ray Pulsars]]

This table attempts to summarize all known cyclotron line sources. It is based on the presentation [http://astrons.sabanciuniv.edu/astrons2010/wordpress/wp-content/uploads/2009/12/Spectral-continua-of-accreting-neutron-star-systems.pdf "Spectral continua of accreting neutron star systems"] by Jörn Wilms at the conference
[http://astrons.sabanciuniv.edu/astrons2010/wordpress/ Astrophysics of Neutron Stars 2010] with some information added later.

T/P = Transient/Persistent

{| class="wikitable"
! #
! Source
! Ecyc [keV]
! Pspin [s]
! Porbital [d]
! Companion
! T/P
! Discovery
|-
|1
| [[Swift J1626.6-5156]]
|10
| 15.4
| 132.9
|Be
|P
|Swift/BAT <ref name="DeCesar09" />
|-
| [[4U 0115+634]]
|14, 24, 36, 48, 62
| 3.6
| 24.3
|Be
|T
|HEAO-1 <ref name="Wheaton79" /> RXTE <ref name="Heindl99" />, BeppoSAX <ref name="Santangelo99" />
|-
| [[4U 1907+09]]
|18, 38
| 441
| 8.37
|B2 III-IV
|P
|BeppoSAX <ref name="Cusumano98b" />
|-
| [[4U 1538-52]]
|22, 47
| 530
| 3.7
|B0I
|P
|Ginga <ref name="Clark90" />, RXTE <ref name="RodesRoca09" />
|-
| [[Vela X-1]]
|24, 52
| 283
| 8.96
|B0.5Ib
|P
|Mir-HEXE <ref name="Kendziorra92" />, RXTE <ref name="Kreykenbohm02" />
|-
| [[V 0332+53]]
|27, 51, 74
| 4.37
| 34.25
|Be
|T
|Ginga <ref name="Makishima90" />
|-
| [[Cep X-4]]
|28
| 66.25
| >23
|B1
|T
|Ginga <ref name="Mihara91" />
|-
| [[Cen X-3]]
|29
| 4.8
| 2.09
|O6.5II
|P
|BeppoSAX <ref name="Santangelo98" />, RXTE <ref name="HeindlChakrabarty99" />
|-
| [[X Per]]
|29?
| 837
| 250.3
|B0 III–Ve
|P
|RXTE <ref name="Coburn01" />
|-
| [[RX J0440.9+4431]]
|32
| 203
| 155
|B0.2 Ve
|T
|INTEGRAL, RXTE + Swift <ref name="Tsygankov12" />
|-
| [[MXB 0656-072]]
|33
| 160
| 100?
|O9.7Ve
|T
|RXTE <ref name="Heindl03b" />
|-
| [[XTE J1946+274]]
|36
| 15.8
| 169.2
|B0-1V-IVe
|T
|RXTE <ref name="Heindl01" />
|-
| [[4U 1626-67]]
|37
| 7.66
| 0.028
|WD?
|P
|BeppoSAX <ref name="Orlandini98b" />, RXTE <ref name="HeindlChakrabarty99" />
|-
| [[GX 301-2]]
|37
| 690
| 41.5
|B1.2Ia
|P
|Ginga <ref name="MiharaPhD" />
|-
| [[Her X-1]]
|41
| 1.24
| 1.7
|A9-B
|P
|Ballon-HEXE <ref name="Truemper78" />
|-
| [[A0535+26]]
|45, 100+
| 104
| 110.6
|Be
|T
|HEXE <ref name="Kendziorra92" /><ref name="Kendziorra94" />, CGRO <ref name="Maisack97" />
|-
| [[1A1118-616]]
|55, 110?
| 408
| 400-800?
|O9.5IV-Ve
|T
|RXTE <ref name="Doroshenko10" />, Suzaku <ref name="Suchy11" />
|-
| [[GRO J1008-57]]
|88?
| 93.7
| 249.46
|B1-B2
|T
|CGRO <ref name="Shrader99" />
|-
| [[GX 304-1]]
|54
| 272
| 132.2
|B2 Vne
|P
|RXTE <ref name="Yamamoto11" />, INTEGRAL <ref name="Klochkov12" />
|-
| [[KS 1947+300]]
|12
| 18.8
| 40.4
|B0Ve
|T
|NuSTAR <ref name="Fuerst14a" />
|}

= Location in the Galaxy =

The figure below displays the position of the sources listed above in the Galaxy as far as known at this moment. Click on the figure for a larger version. Labels indicate the ordinal number in the first column of the table. Uncertainties in the distances are not indicated. Empty symbols represent sources for which there is no distance info in the literature; they have been artificially set to a distance
of 7.6 kpc. The spiral arms are from <ref name="Vallee08" />. Figure and data provided by Arash Bodaghee, SSL, UC Berkeley.

{| class="wikitable"
!
! #
! Source
! Dist. [kpc]
! Reference
|-
|rowspan="17"|[[File:cyclotronlinesourcesinthegalaxy.png|464px]]
| 1
| [[Swift J1626.6-5156]]
| 8±2.4
| <ref name="Reig11b" />
|-
| 2
| [[4U 0115+634]]
| 8±1
| <ref name="Negueruela01" />
|-
| 3
| [[4U 1907+09]]
| 5
| <ref name="Cox05" />
|-
| 4
| [[4U 1538-52]]
| 6.4±1
| <ref name="Reynolds92" />
|-
| 5
| [[Vela X-1]]
|1.4±0.5
| <ref name="ChevalierIlovaisky98" />
|-
| 6
| [[V 0332+53]]
|7.5±1.5
| <ref name="Negueruela99" />
|-
| 7
| [[Cep X-4]]
|3.8±0.6
| <ref name="BonnetBidaudMouchet98" />
|-
| 8
| [[Cen X-3]]
|10±1
| <ref name="Hutchings79" />
|-
| 9
| [[X Per]]
|0.7±0.3
| <ref name="Lyubimkov97" />
|-
| 10
| [[MXB 0656-072]]
|3.9±0.1
| <ref name="McBride06" />
|-
| 11
| [[XTE J1946+274]]
|9.5±2.9
| <ref name="Wilson03" />
|-
| 12
| [[4U 1626-67]]
|9
| <ref name="GrimmGilfanovSunyaev02" />
|-
| 13
| [[GX 301-2]]
|4.1
| <ref name="Leahy02a" />
|-
| 14
| [[Her X-1]]
|6.6±0.4
| <ref name="Reynolds97" />
|-
| 15
| [[A0535+26]]
|2-0.7+0.4
| <ref name="Steele98" />
|-
| 16
| [[1A1118−61]]
|5±2
| <ref name="JanotPacheco81" />
|-
| 17
| [[xrp:gro_j1008-57|GRO J1008−57]]
|5
| <ref name="GrimmGilfanovSunyaev02" />
|}

= References =

Skivergnuegen 2022

2022-01-15T12:12:12Z

Sokolova-lapa: /* Aufteilung */

'''Remeis Skifahren 2022''' The same procedure as every year ;-)
Hier werden die wichtigsten organisatorischen Dinge festgehalten. Jeder darf hier gerne editieren; wer keinen Account für das Wiki hat, muss sich bitte an jemanden wenden, der Zugang hat.

[[File:154854 silvretta-montafon-panorama.jpeg|right|700px]]

== Allgemeine Infos ==

*Ferienwohnung(en):
**Wir kommen wieder unter im [https://www.grandau.at/montafon/zimmer/ferienhaus-enzian Haus Enzian] des [https://www.grandau.at/ Sporthotels Grandau].
**Adresse des Sporthotel: Montafonerstraße 274a, 6791 St. Gallenkirch, Österreich. Unsere Unterkünfte liegen im Türkeiweg.

*Skigebiet: Montafon (Vorarlberg)
**Skigebiet Karte: https://winter.intermaps.com/montafon?lang=de
**Skipass Preise: https://www.montafon.at/de/Service/Bergbahn-Preise-Tickets/Mehrtageskarte-Winter
**Wer nicht alle 7 Tage Skifahren möchte: Es gibt Angebote wie z.B. 5 aus 7, mit einem solchen Skipass kann man innerhalb von 7 Tagen an 5 beliebigen Tagen skifahren.

*Skiverleih: [http://www.sportharry.at/ Sport Harry], direkt an der Talstation.

== Unterkunft ==
=== Aufteilung ===

Dieses Jahr gibt es nur die Hütte mit folgenden Zimmern (wir sind insgesamt 12, also bleiben 2 Plätze frei).

{| class="wikitable"
! scope="col" | Zimmer
! scope="col" | Insassen
|-
! scope="row" | 2-er

|-
! scope="row" | 3-er
| Thomas
|-
! scope="row" | 4-er
| Max, Philipp, Jakob, Katya
|-
! scope="row" | 5-er
| Eva, Steffen, Nela, Ohle, Flo?
|}

== Fahrer ==
Fahrer können sich hier eintragen und Eckdaten angeben. Diejenige, die mitfahren möchten, sprechen sich mit den Fahrern ab und tragen sich ebenfalls ein. Klärt bitte auch die Gepäcklage, ggf. kann ein anderer Fahrer z.B. Skiausrüstung mitnehmen.

'''Auf der Suche nach einer Mitfahrgelegenheit: '''

{| class="wikitable"
! scope="col" | Fahrer
! scope="col" | # Plätze
! scope="col" | Anreise
! scope="col" | Mitfahrer Anreise
! scope="col" | Abreise
! scope="col" | Mitfahrer Abreise
! scope="col" | Skimitnahme
! scope="col" | Kommentar
|-
|Eva
|0(3)
|Samstag
|Steffen+Christian
|Samstag?
|Steffen+Christian
|eigene ja
|Auto is voll
|-
|Johannes
|1+x(2+x?)
|Samstag
|
|Samstag?
|
|ja
|Mietwagen, daher noch x Plätze mehr möglich
|-
|Flo
|3(4)
|Samstag
|
|Samstag?
|
|ja
|fährt von Minga
|-
|Max
|4
|Samstag
|Katya, Jakob, Philipp
|Samstag?
|Katya, Jakob, Philipp
|ja
|voll, fährt von Erlangen
|-
|Nela
|1(2) ??
|Samstag
|Ohle
|Samstag?
|
|?
|
|-
|}

== Schwarzes Brett ==

=== Essen ===
Hier gibt's den Essensplan, soweit übernommen von den letzten Jahren. Da wir sehr viele Leute sind, sollten wir wieder vorab grob planen, was wir kochen wollen. Wir können einige Dinge in Deutschland besorgen und mitnehmen, es gib aber auch einen nahe gelegen Supermarkt. Generelle Dinge, wie z.B. Gewürze oder Aufstriche für Frühstücksbrötchen könnte man auch mitbringen.

Wer Kochvorschläge oder andere Ideen hat, gerne unten eintragen und kommentieren. Bedenkt, dass die Zubereitung (relativ) einfach sein sollte. Da sich die Liste in den letzten Jahren gut bewaehrt hat, behalten wir sie bei, aber die Reihenfolge/Tage kann man sicher noch hin und her bewegen. Einige (wenige) Sachen müssen wir dann manchmal trotzdem noch beim Spar kaufen, da ja auch der Kühlschrank nur begrenzt Platz hat.

'''Essenplan:'''
*Samstag: Spaghetti Bolognese + veg. Bolognese
*Sonntag: Käse Spätzle
*Montag: Burritos
*Dienstag: Risotto
*Mittwoch: Gulasch
*Donnerstag: Kartoffeln mit Kräuter-Quark
*Freitag: Dal mit Reis (od. Curry mit Suesskartoffeln )

Einkaufsliste hier: https://docs.google.com/document/d/166b_mIXxmoAgcv1upIGremd_36E1fmwwxsQADP2uEv8/

@Christian: Vegane Option entwender selbst mitbringen oder hier mit reinschreiben (falls man die einfach bekommt)

=== Alkohol/Party ===

=== Spiele ===

Immer lustig sind gemeinsame Spieleabende. Also, wer im Besitz von Gesellschaftsspielen ist, bringt diese gerne mit! Um eine Übersicht zu bekommen auch bitte hier eintragen:

''* Spiele hier eintragen''

=== Sonstiges ===

=== Alternativprogramm ===
* Rodeln (http://www.montafon.at/de/urlaubswelten/echte_naturliebhaber/rodeln)
* Schneeschuhwandern (http://www.montafon.at/schneeschuhwanderungen)
* Therme (http://www.montafon.at/schwimmen), z.B. http://www.aqua-dome.at/de (ca. 130km entfernt!)

[[Category:Internal]]

Model decomp (xfig example)

2018-05-02T11:23:57Z

Sokolova-lapa:

[[Category:SLxfig]]

[[File:multipanel_decomposition.png|800px|]]

Spectral data and models of the best fits have been stored in tables using write_plot() and eval_fun_keV() in a file structure of shape /userdata/data/user/ "source" / "model" /decomposition/ "component"

<pre>
#!/usr/bin/env isis-script

require("isisscripts");

variable COLOR = ["dimgray","darkgray","lightgrey"];
variable MCOLOR = ["darkorange","blue","mediumaquamarine","purple","black"];

% Lists of object names and model components to automatically build data paths
variable comp_list = {"tbnew_feo*relxilllp","tbnew_feo*powerlaw","tbnew_feo*xillver","complete_model","absorbed_model"};
variable namelist = {"ark120","pds456","fairall9", "ngc1365", "3c390_3", "3c382"};
variable tex_name = {"Ark 120","PDS 456","Fairall 9", "NGC 1365", "3C390.3", "3C382"};
variable detconst = {{1,1/1.08,1/1.1},{1,1/0.68,1/0.75},{1,1/0.995,1/1.02},{1,1/0.96,1/0.98},{1,1/1.062567,1/1.115621},{1,1/0.8153,1/0.7853389}};

%-------main-loop-over-namelist---------------
variable panel = Struct_Type[length(namelist)];
variable i,j, lo, hi, val, err, err_max, err_min;

for(j=0;j<length(namelist);j++){

% initialize panel j
panel[j] = xfig_plot_new(12, 9);
panel[j].world(0.5,80,5e-08,0.1; xlog=1, ylog=1);
panel[j].ylabel(`Flux \footnotesize[s$^{-1}$\,cm$^{-2}$\,keV$^{-1}$]`);
panel[j].xylabel(0.95,0.9,tex_name[j],0.5,0; world0);

variable write_folder = "/userdata/data/fink/"+namelist[j]+"/fit_relxilllp/decomposition/";

% plot data from three detectors in the background, corrected for according detector constant
for(i=0;i<=2;i++){
(lo, hi, val, err) = readcol(write_folder+"data_"+string(i)+".dat", 1, 2, 3, 4);
panel[j].plot((lo+hi)/2., val*detconst[j][i], err*detconst[j][i]; sym="point", size=-1, eb_factor=0, color=COLOR[i]);
}

% plot model components (exception for pds456)
for(i=0;i<length(comp_list);i++){
if(not(comp_list[i]=="tbnew_feo*xillver" && namelist[j] == "pds456")){
(lo, hi, val) = readcol(write_folder+comp_list[i]+".dat", 1, 2, 3);
panel[j].plot((lo+hi)/2, val; line=0, eb_factor=0, size=0.01, color=MCOLOR[i], depth=10-i);
}
}
}

% some model labels
variable ypos = 0.42, ystep = 0.08;
panel[1].xylabel(0.05, ypos - 0*ystep, "Powerlaw", -0.5, 0; world0, color = MCOLOR[1]);
panel[1].xylabel(0.05, ypos - 1*ystep, "CDR",-0.5,0; world0, color = MCOLOR[2]);
panel[1].xylabel(0.05, ypos - 2*ystep, "Lamppost-RR",-0.5,0; world0, color = MCOLOR[0]);
panel[1].xylabel(0.05, ypos - 3*ystep, "Powerlaw + Reflection",-0.5,0; world0, color = MCOLOR[3]);
panel[1].xylabel(0.05, ypos - 4*ystep, "Full Absorbed Model",-0.5,0; world0, color = MCOLOR[4]);

%---------render-all--------------
variable multi = xfig_multiplot(panel; xlabel=`Energy [keV]`, cols=2);
multi.render("multipanel_decomposition.pdf");

quit;
</pre>

Object3dsimple (xfig example)

2018-05-02T11:23:28Z

Sokolova-lapa:

[[Category:SLxfig]]
===== Polar plot with 'xfig_polarplot_new =====

[[File:object3dsimple.png|300px|]]

<pre>
require("isisscripts");
%%%%% GLOBAL PARAMETER: =======================================================

xfig_set_latex_preamble("\renewcommand{\vec}[1]{\ensuremath{\mathbf{#1}}}"R);

%%% CAMERA: modified Spherical angles
variable cam1 = 20*PI/180.; % cam1 = PI/2 - thetaa
variable cam2 = -20*PI/180.; % cam2 = PI - phi

%%% GEOMETRY:
variable theta = 60*PI/180.; % Spot position
variable phi = 35*PI/180.; % Spot position
variable R = 1;

%%% PLOT DIMENSION
variable size = 18;
variable xmin = -0.50*R;
variable xmax = 2.20*R;
variable ymin = -0.175*R;
variable ymax = 2.10*R;

%%% PLOT COLORS
variable col_cbg = ["#88CCEE",
"#999933",
"#AA4499",
"#332288"
];
variable emitter = CB_COLOR_SCHEME[3];
variable intens = CB_COLOR_SCHEME[4];
variable mu = CB_COLOR_SCHEME[5];
variable muS = CB_COLOR_SCHEME[6];

%%% PHYSICAL VECTORS ==========================================================

%%% CAMERA: Basis vectors
variable c1 = vector(1,0,0);
variable c2 = vector(0,1,0);
variable c3 = vector(0,0,1);

c1 = vector_rotate( c1, vector(0,0,1), cam2 );
c2 = vector_rotate( c2, vector(0,0,1), cam2 );
c3 = vector_rotate( c3, vector(0,0,1), cam2 );
c1 = vector_rotate( c1, vector(1,0,0), cam1 );
c2 = vector_rotate( c2, vector(1,0,0), cam1 );
c3 = vector_rotate( c3, vector(1,0,0), cam1 );

%%% AXIS
variable ex = vector( R, 0, 0 );
variable ey = vector( 0, R, 0 );
variable ez = vector( 0, 0, R );

%%% PHOTON
variable k0 = vector( (1+2*sin(theta)*cos(phi))/3., phi, theta ; sph );
variable k0xy= @k0; k0xy.z=0;
variable k0x= @k0; k0x.y=0;k0x.z=0;
variable k0z= @k0; k0z.x=0;k0z.y=0;

%%% FUNCTIONS =================================================================
%%% Must be defined here, as functions require some global variables!

% Projection of vectors onto the camera plane
define P( v ){ %{{{
variable vec = @v;
if( typeof(vec)== Array_Type ){
vec = merge_struct_arrays( v );
}
variable pro = vector_change_basis( vec, c1, c2, c3 );
return pro;
}
%}}}
% Return x,z component of Projection
define PP( v ){ %{{{
variable p = P(v);
return p.x, p.z;
}
%}}}
% GREAT CIRCLE between 2 Vector
define GC( a, b ){ %{{{

variable N = qualifier("N",100);
variable R = qualifier_exists("R")? 1:0;

variable na = unit_vector(a);
variable nb = unit_vector(b);

variable rotangle = [0:acos(dotprod(na,nb))-R*2*PI:#N];
variable rotvec = unit_vector( crossprod( a, b ) );

variable gc = vector_rotate( na, rotvec, rotangle );

return gc;
}
%}}}

%%% PREPARE PLOT ==============================================================
variable s = 1.1;
variable ls= s*1.06;
variable N = 50;

% arrow head
variable ARROW = xfig_create_arrow(;arrow_type=2,
arrow_style=1,
arrow_width=8,
arrow_heigth=64,
arrow_thickness=2
);
variable AXIS = @ARROW;
AXIS.arrow_style=0;
AXIS.arrow_type=0;

% intensity profile
variable xyint1 = vector( [0,(1+2*cos([-PI/2: 0:#N]))/3.], [0,[-PI/2: 0:#N]], [0,[PI/2.:PI/2.:#N]]; sph );
variable xyint2 = vector( [(1+2*cos([ 0: PI/2:#N]))/3.,0], [[ 0: PI/2:#N],0], [[PI/2.:PI/2.:#N],0]; sph );
variable xzint1 = vector( [0,(1+2*sin([ 0: PI/2:#N]))/3.], [0,[ 0: 0:#N]], [0,[0 : PI/2:#N]]; sph );
variable xzint2 = vector( [(1+2*sin([ PI/2: PI:#N]))/3.,0], [[ 0: 0:#N],0], [[PI/2 : PI:#N],0]; sph );
variable yzint = vector( (1+2*cos([-PI/2:-PI/2:#N]))/3., [-PI/2:-PI/2:#N], [0 :2.*PI:#N]; sph );

% mu: eta angle
variable eta = .3*GC( k0, k0z );
variable etaS = .3*GC( k0x, k0xy );

%%% PLOT ======================================================================
variable xp = xfig_plot_new(size,(ymax-ymin)/(xmax-xmin)*size);
xp.world( xmin, xmax, ymin, ymax ; padx=0.0, pady=0.0 );
xp.axis(;off);

% axis
xp.plot( PP([0,s]*R*ex); forward_arrow=AXIS );
xp.xylabel( PP(ls*R*ex), "$\vec{e}_\mathsf{S}$"R );

% xp.plot( PP([0,s]*R*ey); forward_arrow=AXIS );
% xp.xylabel( PP(ls*ey), "$y$"R );

xp.plot( PP(.5*[0,s]*ez); forward_arrow=AXIS );
xp.xylabel( PP(.5*ls*ez), "$\vec{e}_\mathsf{B}$"R );

% ZERO
xp.plot( PP(0.01*yzint) ; width=4, depth=10 );

% k0
xp.plot( PP([0,1]*k0); width=2, forward_arrow=ARROW );
xp.xylabel( PP(1.1*k0), "$\vec{k}'$"R );

% k0 components
xp.plot( PP([0,1]*k0xy); width=2 );

xp.plot( PP([k0z,k0]) ; width=2, line=1 );
xp.plot( PP([k0xy,k0]) ; width=2, line=1 );
xp.plot( PP([k0xy,k0x]); width=2, line=1 );
xp.plot( PP([k0z,k0z+k0x]); width=2, line=2 );
xp.plot( PP([k0x,k0z+k0x]); width=2, line=2 );
xp.plot( PP([k0,k0z+k0x]); width=2, line=2 );

% angles
xp.plot( PP(eta) ; width=2, line=0 );
xp.xylabel( PP(0.75*vector(mean(eta.x),mean(eta.y),mean(eta.z))), "$\eta'$"R );
xp.plot( PP(etaS) ; width=2, line=0 );
xp.xylabel( PP(1.25*vector(mean(etaS.x),mean(etaS.y),mean(etaS.z))), "$\eta_\mathsf{S}$"R );

% mus
xp.plot( PP([0,1]*k0x) ; width=4, color=muS );
xp.xylabel( PP(.9*k0x-.15*ey), "$\mu_\mathsf{S}$"R ; color=muS );
xp.plot( PP([0,1]*k0z) ; width=4, color=mu );
xp.xylabel( PP(.9*k0z-.15*ey), "$\mu'$"R ; color=mu );

% intensity
xp.plot( PP(xyint1) ; color=intens, line=0, width=2, depth=201 );
xp.plot( PP(xyint2) ; color=intens, line=0, width=2, depth=203 );
xp.plot( PP(xyint2) ; color=intens, line=1, width=1, depth=200 );

xp.plot( PP(xzint1) ; color=intens, line=0, width=2, depth=201 );
xp.plot( PP(xzint2) ; color=intens, line=0, width=2, depth=202 );
xp.plot( PP(xzint2) ; color=intens, line=1, width=1, depth=200 );

xp.plot( PP(yzint) ; color=intens, line=0, width=2, depth=204 );
xp.plot( PP(yzint) ; color=intens, line=1, width=1, depth=200 );

xp.shade_region( PP(xyint1) ; color=intens, fill=36, width=0, depth=201 );
xp.shade_region( PP(xyint2) ; color=intens, fill=36, width=0, depth=203 );
xp.shade_region( PP(xzint1) ; color=intens, fill=36, width=0, depth=201 );
xp.shade_region( PP(xzint2) ; color=intens, fill=36, width=0, depth=202 );
xp.shade_region( PP(yzint) ; color=intens, fill=36, width=0, depth=204 );

% emitter plane
variable eplane = .5*R*vector( [ [ 0: 0:#N], [ 0: 0:#N],[ 0: 0:#N],[ 0: 0:#N]],
[ [-1: 1:#N], [ 1: 1:#N],[ 1:-1:#N],[-1:-1:#N]],
[ [-1:-1:#N], [-1: 1:#N],[ 1: 1:#N],[ 1:-1:#N]]
);
xp.shade_region( PP(eplane); color=emitter, fill=36,depth=250, width=0 );
xp.plot( PP(eplane); color=emitter, line=0, depth=205, width=1 );
xp.plot( PP(eplane); color=emitter, line=1, depth=200, width=1 );

xp.render("bdsframe.pdf");

</pre>

Object3dsimple (xfig example)

2018-05-02T11:21:58Z

Sokolova-lapa: Created page with " Category:SLxfig ===== Polar plot with 'xfig_polarplot_new ===== File:object3dsimple.png <pre> require("isisscripts"); %%%%% GLOBAL PARAMETER: =====================..."

[[Category:SLxfig]]
===== Polar plot with 'xfig_polarplot_new =====

[[File:object3dsimple.png]]

<pre>
require("isisscripts");
%%%%% GLOBAL PARAMETER: =======================================================

xfig_set_latex_preamble("\renewcommand{\vec}[1]{\ensuremath{\mathbf{#1}}}"R);

%%% CAMERA: modified Spherical angles
variable cam1 = 20*PI/180.; % cam1 = PI/2 - thetaa
variable cam2 = -20*PI/180.; % cam2 = PI - phi

%%% GEOMETRY:
variable theta = 60*PI/180.; % Spot position
variable phi = 35*PI/180.; % Spot position
variable R = 1;

%%% PLOT DIMENSION
variable size = 18;
variable xmin = -0.50*R;
variable xmax = 2.20*R;
variable ymin = -0.175*R;
variable ymax = 2.10*R;

%%% PLOT COLORS
variable col_cbg = ["#88CCEE",
"#999933",
"#AA4499",
"#332288"
];
variable emitter = CB_COLOR_SCHEME[3];
variable intens = CB_COLOR_SCHEME[4];
variable mu = CB_COLOR_SCHEME[5];
variable muS = CB_COLOR_SCHEME[6];

%%% PHYSICAL VECTORS ==========================================================

%%% CAMERA: Basis vectors
variable c1 = vector(1,0,0);
variable c2 = vector(0,1,0);
variable c3 = vector(0,0,1);

c1 = vector_rotate( c1, vector(0,0,1), cam2 );
c2 = vector_rotate( c2, vector(0,0,1), cam2 );
c3 = vector_rotate( c3, vector(0,0,1), cam2 );
c1 = vector_rotate( c1, vector(1,0,0), cam1 );
c2 = vector_rotate( c2, vector(1,0,0), cam1 );
c3 = vector_rotate( c3, vector(1,0,0), cam1 );

%%% AXIS
variable ex = vector( R, 0, 0 );
variable ey = vector( 0, R, 0 );
variable ez = vector( 0, 0, R );

%%% PHOTON
variable k0 = vector( (1+2*sin(theta)*cos(phi))/3., phi, theta ; sph );
variable k0xy= @k0; k0xy.z=0;
variable k0x= @k0; k0x.y=0;k0x.z=0;
variable k0z= @k0; k0z.x=0;k0z.y=0;

%%% FUNCTIONS =================================================================
%%% Must be defined here, as functions require some global variables!

% Projection of vectors onto the camera plane
define P( v ){ %{{{
variable vec = @v;
if( typeof(vec)== Array_Type ){
vec = merge_struct_arrays( v );
}
variable pro = vector_change_basis( vec, c1, c2, c3 );
return pro;
}
%}}}
% Return x,z component of Projection
define PP( v ){ %{{{
variable p = P(v);
return p.x, p.z;
}
%}}}
% GREAT CIRCLE between 2 Vector
define GC( a, b ){ %{{{

variable N = qualifier("N",100);
variable R = qualifier_exists("R")? 1:0;

variable na = unit_vector(a);
variable nb = unit_vector(b);

variable rotangle = [0:acos(dotprod(na,nb))-R*2*PI:#N];
variable rotvec = unit_vector( crossprod( a, b ) );

variable gc = vector_rotate( na, rotvec, rotangle );

return gc;
}
%}}}

%%% PREPARE PLOT ==============================================================
variable s = 1.1;
variable ls= s*1.06;
variable N = 50;

% arrow head
variable ARROW = xfig_create_arrow(;arrow_type=2,
arrow_style=1,
arrow_width=8,
arrow_heigth=64,
arrow_thickness=2
);
variable AXIS = @ARROW;
AXIS.arrow_style=0;
AXIS.arrow_type=0;

% intensity profile
variable xyint1 = vector( [0,(1+2*cos([-PI/2: 0:#N]))/3.], [0,[-PI/2: 0:#N]], [0,[PI/2.:PI/2.:#N]]; sph );
variable xyint2 = vector( [(1+2*cos([ 0: PI/2:#N]))/3.,0], [[ 0: PI/2:#N],0], [[PI/2.:PI/2.:#N],0]; sph );
variable xzint1 = vector( [0,(1+2*sin([ 0: PI/2:#N]))/3.], [0,[ 0: 0:#N]], [0,[0 : PI/2:#N]]; sph );
variable xzint2 = vector( [(1+2*sin([ PI/2: PI:#N]))/3.,0], [[ 0: 0:#N],0], [[PI/2 : PI:#N],0]; sph );
variable yzint = vector( (1+2*cos([-PI/2:-PI/2:#N]))/3., [-PI/2:-PI/2:#N], [0 :2.*PI:#N]; sph );

% mu: eta angle
variable eta = .3*GC( k0, k0z );
variable etaS = .3*GC( k0x, k0xy );

%%% PLOT ======================================================================
variable xp = xfig_plot_new(size,(ymax-ymin)/(xmax-xmin)*size);
xp.world( xmin, xmax, ymin, ymax ; padx=0.0, pady=0.0 );
xp.axis(;off);

% axis
xp.plot( PP([0,s]*R*ex); forward_arrow=AXIS );
xp.xylabel( PP(ls*R*ex), "$\vec{e}_\mathsf{S}$"R );

% xp.plot( PP([0,s]*R*ey); forward_arrow=AXIS );
% xp.xylabel( PP(ls*ey), "$y$"R );

xp.plot( PP(.5*[0,s]*ez); forward_arrow=AXIS );
xp.xylabel( PP(.5*ls*ez), "$\vec{e}_\mathsf{B}$"R );

% ZERO
xp.plot( PP(0.01*yzint) ; width=4, depth=10 );

% k0
xp.plot( PP([0,1]*k0); width=2, forward_arrow=ARROW );
xp.xylabel( PP(1.1*k0), "$\vec{k}'$"R );

% k0 components
xp.plot( PP([0,1]*k0xy); width=2 );

xp.plot( PP([k0z,k0]) ; width=2, line=1 );
xp.plot( PP([k0xy,k0]) ; width=2, line=1 );
xp.plot( PP([k0xy,k0x]); width=2, line=1 );
xp.plot( PP([k0z,k0z+k0x]); width=2, line=2 );
xp.plot( PP([k0x,k0z+k0x]); width=2, line=2 );
xp.plot( PP([k0,k0z+k0x]); width=2, line=2 );

% angles
xp.plot( PP(eta) ; width=2, line=0 );
xp.xylabel( PP(0.75*vector(mean(eta.x),mean(eta.y),mean(eta.z))), "$\eta'$"R );
xp.plot( PP(etaS) ; width=2, line=0 );
xp.xylabel( PP(1.25*vector(mean(etaS.x),mean(etaS.y),mean(etaS.z))), "$\eta_\mathsf{S}$"R );

% mus
xp.plot( PP([0,1]*k0x) ; width=4, color=muS );
xp.xylabel( PP(.9*k0x-.15*ey), "$\mu_\mathsf{S}$"R ; color=muS );
xp.plot( PP([0,1]*k0z) ; width=4, color=mu );
xp.xylabel( PP(.9*k0z-.15*ey), "$\mu'$"R ; color=mu );

% intensity
xp.plot( PP(xyint1) ; color=intens, line=0, width=2, depth=201 );
xp.plot( PP(xyint2) ; color=intens, line=0, width=2, depth=203 );
xp.plot( PP(xyint2) ; color=intens, line=1, width=1, depth=200 );

xp.plot( PP(xzint1) ; color=intens, line=0, width=2, depth=201 );
xp.plot( PP(xzint2) ; color=intens, line=0, width=2, depth=202 );
xp.plot( PP(xzint2) ; color=intens, line=1, width=1, depth=200 );

xp.plot( PP(yzint) ; color=intens, line=0, width=2, depth=204 );
xp.plot( PP(yzint) ; color=intens, line=1, width=1, depth=200 );

xp.shade_region( PP(xyint1) ; color=intens, fill=36, width=0, depth=201 );
xp.shade_region( PP(xyint2) ; color=intens, fill=36, width=0, depth=203 );
xp.shade_region( PP(xzint1) ; color=intens, fill=36, width=0, depth=201 );
xp.shade_region( PP(xzint2) ; color=intens, fill=36, width=0, depth=202 );
xp.shade_region( PP(yzint) ; color=intens, fill=36, width=0, depth=204 );

% emitter plane
variable eplane = .5*R*vector( [ [ 0: 0:#N], [ 0: 0:#N],[ 0: 0:#N],[ 0: 0:#N]],
[ [-1: 1:#N], [ 1: 1:#N],[ 1:-1:#N],[-1:-1:#N]],
[ [-1:-1:#N], [-1: 1:#N],[ 1: 1:#N],[ 1:-1:#N]]
);
xp.shade_region( PP(eplane); color=emitter, fill=36,depth=250, width=0 );
xp.plot( PP(eplane); color=emitter, line=0, depth=205, width=1 );
xp.plot( PP(eplane); color=emitter, line=1, depth=200, width=1 );

xp.render("bdsframe.pdf");

</pre>

Object3d (xfig example)

2018-05-02T11:19:17Z

Sokolova-lapa: Created page with " Category:SLxfig ===== Plotting in 3D ===== <pre> % -*- mode: slang; mode: fold -*- require("isisscripts"); require("lbscripts"); ()=evalfile("/home/falkner/work/lightbe..."

[[Category:SLxfig]]

===== Plotting in 3D =====
<pre>
% -*- mode: slang; mode: fold -*-
require("isisscripts");
require("lbscripts");
()=evalfile("/home/falkner/work/lightbending/lbscripts.git/modules/ptrace.sl");

%%%%% GLOBAL PARAMETER: =======================================================

xfig_set_latex_preamble("\renewcommand{\vec}[1]{\ensuremath{\mathbf{#1}}}"R);

%%% CAMERA: modified Spherical angles
variable cam1 = 20*PI/180.; % cam1 = PI/2 - thetaa
variable cam2 = 0*PI/180.; % cam2 = PI - phi

%%% LIGHT BENDING:
variable Mns = 1.44*2e30;
%variable Rns = 10e3; % Physical radius of the neutron star
variable rs = 2*Const_G*Mns/sqr(Const_c)*1e1; % Schwarzschild radius
variable r = 15e3; % radius of photon emission
variable u = rs/r;

%%% GEOMETRY:
variable R = 1; % radius of the sphere [BUG HERE FOR R /= 1]

variable i = 60*PI/180.; % Inclination of the observer

variable theta = 45*PI/180.; % Spot position
variable phi = 220*PI/180.; % Spot position

%%% PLOT DIMENSION
variable size = 12;
variable xmin = -1.00*R;
variable xmax = 2.20*R;
variable ymin = -0.55*R;
variable ymax = 2.10*R;

%%% PLOT COLORS
variable col_cbg = ["#88CCEE",
"#999933",
"#AA4499",
"#332288"
];
% variable photon1 = col_cbg[2];
% variable photon2 = col_cbg[3];
% variable obsplane = col_cbg[1];
variable photon1 = CB_COLOR_SCHEME[1];
variable photon2 = CB_COLOR_SCHEME[2];
variable obsplane = "#505050";

%%% PHYSIKAL VECTORS ==========================================================

%%% CAMERA: Basis vectors
variable c1 = vector_rotate( vector(1,0,0), vector(1,0,0), cam1 );
variable c2 = vector_rotate( vector(0,1,0), vector(1,0,0), cam1 );
variable c3 = vector_rotate( vector(0,0,1), vector(1,0,0), cam1 );
c1 = vector_rotate( c1, vector(0,0,1), cam2 );
c2 = vector_rotate( c2, vector(0,0,1), cam2 );
c3 = vector_rotate( c3, vector(0,0,1), cam2 );

%%% AXIS
variable ex = vector( R, 0, 0 );
variable ey = vector( 0, R, 0 );
variable ez = vector( 0, 0, R );

%%% OBSERVER
variable k = vector( sin(i), 0, cos(i) );
%%% SPOT
variable n = vector( 1, phi, theta ; sph );

%%% LIGHT BENDING CALCULATIONS
%%% Attention: simple calculations based on beloborodov 2002, i.e., it
%%% does not work for all settings (where alpha > 90°)

variable lbpar = struct{
nmr = 10,
nma = 100,
rmin = 0.95*r/rs,
rmax = 1.05*r/rs,
lbmeth = "belob",
tdelay=0,
};
variable lbmap = lb_psir2b_map( lbpar );

%% Solution 1:
variable psi = acos( dotprod(k,n) );
variable alpha = acos( 1 - ( 1-cos(psi) )*( 1-u ) );
alpha = lb_interp( lbmap, r/rs, psi, struct{ a, b } ).a;

variable b = R*sin(alpha)/sqrt(1-u);
b = lb_interp( lbmap, r/rs, psi, struct{ a, b } ).b*rs/r*R;

variable crho = ( ( k^(n^k) ) * ey )/abs( k^(n^k) );
variable srho = abs( ( k^(n^k) ) ^ ey )/abs( k^(n^k) );

variable k0 = unit_vector(vector_rotate( n, crossprod(n,k), alpha ));

%% Solution 2:
%% 1 - cos(alpha) = ( 1 - cos(psi) )*(1-u)
%% b = R*sin(alpha) / sqrt(1-u)
variable _psi = 2*PI - psi;
variable _alpha = acos( 1 - ( 1-cos(_psi) )*( 1-u ) );;
_alpha = lb_interp( lbmap, r/rs, _psi, struct{ a, b } ).a;

variable fac = rs/r*R;
variable _b = R*sin(_alpha)/sqrt(1-u);
_b = lb_interp( lbmap, r/rs, _psi, struct{ a, b } ).b*fac;
variable _rp = lb_p_b( _b/fac )*fac;
variable _pp = lb_psiper_u_belob_( fac/_rp );

variable _k0 = unit_vector(vector_rotate( n, crossprod(n,k), -_alpha ));

%%% FUNCTIONS =================================================================
%%% Must be defined here, as functions require some global variables!

% Projection of vectors onto the camera plane
define P( v ){ %{{{
variable vec = @v;
if( typeof(vec)== Array_Type ){
vec = struct_array_2_struct_of_arrays( v );
}
variable pro = vector_change_basis( vec, c1, c2, c3 );
return pro;
}
%}}}
% Return x,z component of Projection
define PP( v ){ %{{{
variable p = P(v);
return p.x, p.z;
}
%}}}
% GREAT CIRCLE between 2 Vector
define GC( a, b ){ %{{{

variable N = qualifier("N",100);
variable R = qualifier_exists("R")? 1:0;

variable na = unit_vector(a);
variable nb = unit_vector(b);

variable rotangle = [0:acos(dotprod(na,nb))-R*2*PI:#N];
variable rotvec = unit_vector( crossprod( a, b ) );

variable gc = vector_rotate( na, rotvec, rotangle );

return gc;
}
%}}}
% PHOTON TRAJECTORY
define T(p){ %{{{
variable B = b/R*r;
variable X = rs*( 1 - cos(p))/(2*( 1 + cos(p)));
variable trace = sqrt( sqr(X) + sqr(B/sin(p)) ) - X;
return trace/r*R;
}
%}}}
define PT(){ %{{{
variable brs = b/R*r/rs;
variable pt = lb_ptrace_belob( brs ; n=N, pmax=psi );

variable v = vector( pt.r*rs/r*R, [0:0:#N], -pt.p ; sph );
v = vector_rotate( v, ey, i );
v = vector_rotate( v, k, -atan2(crho,srho) );

return v;
}
%}}}
define _PT(){ %{{{
variable brs = _b/R*r/rs;

variable pt = lb_ptrace_belob( brs ; n=N, pmax=2*PI-psi );

variable v = vector( pt.r*rs/r*R, [0:0:#N], -pt.p ; sph );
v = vector_rotate( v, ey, i );
v = vector_rotate( v, k, PI-atan2(crho,srho) );

return v;
}
%}}}

%%% PREPARE PLOT ==============================================================
variable s = 1.5;
variable ls= s*1.06;
variable N = 300;

% arrow head
variable ARROW = xfig_create_arrow(;arrow_type=2,
arrow_style=1,
arrow_width=8,
arrow_heigth=64,
arrow_thickness=2
);
variable AXIS = @ARROW;
AXIS.arrow_style=0;
AXIS.arrow_type=0;

% circle
variable xycirc = vector( [R:R:#N], [0:2*PI:#N], [PI/2.:PI/2.:#N]; sph );
variable xzcircn = vector( [R:R:#N], [0:0:#N], PI/2.*[-1:1:#N]; sph );
variable xzcircs = vector( [R:R:#N], [0:0:#N], PI/2.*[1:3:#N]; sph );

% n help lines
variable ncirc = vector( [R:R:#N], [phi:phi:#N], [0:PI/2:#N]; sph );
variable nline = vector( [0:R:#N], [phi:phi:#N], [PI/2:PI/2:#N];sph);

% kn circ
variable kncirc = R*GC( unit_vector(n), unit_vector(k) );
variable nkcirc = R*GC( unit_vector(n), unit_vector(k) ; R );

%%% PLOT ======================================================================
variable xp = xfig_plot_new(size,(ymax-ymin)/(xmax-xmin)*size);
xp.world( xmin, xmax, ymin, ymax ; padx=0.0, pady=0.0 );
xp.axis(;off);

% axis
xp.plot( PP([0,s]*R*ex); forward_arrow=AXIS );
xp.xylabel( PP(ls*R*ex), "$x$"R );

xp.plot( PP([0,s]*ey) );
%xp.xylabel( PP(ls*ey), "$y$"R );

xp.plot( PP([0,s]*R*ez); forward_arrow=AXIS );
xp.xylabel( PP(ls*ez), "$z$"R );

% circles
xp.plot( PP(xzcircn) ; line=0, width=2 );
xp.plot( PP(xzcircs) ; line=0, width=2 );
xp.plot( PP(xycirc) ; line=0, width=2 );

% rotation
variable rot = 0.8*s*R*ez+vector( 0.15*[R:R:#N], PI/180*[-60:265:#N], [PI/2.:PI/2.:#N]; sph );
xp.plot( PP(rot); forward_arrow=AXIS );

% observer
xp.plot( PP([0,1]*R*k) ; line=1 );
xp.plot( PP([1,s]*R*k) ; line=0 );
xp.xylabel( PP(ls*k), "$\vec{k}$"R, 1.5, 1.5 );
xp.plot( PP([1,s]*R*k); forward_arrow=ARROW );

% observer plane
variable deltap = 1.8*R;
variable oplane = 1.2*R*vector( [-1, 1, 1,-1,-1],
[-1,-1, 1, 1,-1],
[ 0, 0, 0, 0, 0]
);
oplane.z += deltap;
oplane = vector_rotate( oplane, ey, i );
xp.plot( PP(oplane); depth=40, width=3, color=obsplane );
%variable oplab = 1.8*R*vector( -.01, -.95, 0 );
variable oplab = 1.8*R*vector( .60, 0, 0 );
oplab.z += deltap;
oplab = vector_rotate( oplab, ey, i );
%xp.xylabel( PP(oplab), "observer plane"R ; rotate=-0.97*i*180/PI, color=obsplane );
xp.xylabel( PP(oplab), "{\footnotesize observer plane}"R ; rotate=90, color=obsplane );
variable ocirc = vector( [R:R:#N],[0:2*PI:#N],PI/2.*[1:1:#N]; sph );
ocirc.z += deltap;
ocirc = vector_rotate( ocirc, ey, i );
xp.plot( PP(ocirc); color=obsplane );
variable A = 1.15*s*R*vector( [0,0],[0,1],[0,0] );
A.z += deltap;
A = vector_rotate( A, ey, i );
xp.plot( PP(A) ; forward_arrow=AXIS, color=obsplane );
xp.xylabel( PP(struct_of_arrays_2_struct_array(A)[-1]), "$A$"R, -.5, 1.2;color=obsplane);
variable B = s*R*vector( [0,-1],[0,0],[0,0] );
B.z += deltap;
B = vector_rotate( B, ey, i );
xp.plot( PP(B) ; forward_arrow=AXIS,color=obsplane );
xp.xylabel( PP(struct_of_arrays_2_struct_array(B)[-1]), "$B$"R, -.4, 2.2;color=obsplane );

%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
%%% IMPACT A & B
%%%%%%%%%%%%%%%%

% Line in OP from center to impact point 1
variable IB = b*vector( [0,1], PI/2+[0,PI/2-atan2(crho,srho)], PI/2*[1,1] ; sph );
variable IB2 = @IB;
IB.z += deltap;
IB = vector_rotate( IB, ey, i );
xp.plot( PP(IB) ; line=1,color=obsplane );
% Projected circle at the impact point 1
variable IBcirc = vector( 0.05*[R:R:#N],[0:2*PI:#N],PI/2.*[1:1:#N]; sph );
IBcirc.z += deltap;
IBcirc = vector_rotate( IBcirc, ey, i );
IBcirc += struct_of_arrays_2_struct_array(IB)[-1] - struct_of_arrays_2_struct_array(IB)[0];
IBcirc = struct_of_arrays_2_struct_array(IBcirc);
%xp.shade_region( PP(IBcirc) ; fillcolor=photon1,width=0);
xp.plot( PP(struct_of_arrays_2_struct_array(IB)[-1]) ; sym="circle", color=photon1,fill, size=0.3*R);

% Arrow between k and photon1 tratecory indicating b
IB2.z += 0.7*deltap;
IB2 = vector_rotate( IB2, ey, i );
xp.plot( PP(IB2) ; line=0 , forward_arrow, backward_arrow, depth=150 );
xp.xylabel( PP(vector( mean(IB2.x), mean(IB2.y), mean(IB2.z) )), "$b$"R, -.4, -.4 );

% Line in OP from center to impact point 2
variable _IB = -_b*vector( [0,1], PI/2+[0,PI/2-atan2(crho,srho)], PI/2*[1,1] ; sph );
_IB.z += deltap;
_IB = vector_rotate( _IB, ey, i );
xp.plot( PP(_IB) ; line=1,color=obsplane );
% Projected circle at the impact point 1
variable _IBcirc = vector( 0.05*[R:R:#N],[0:2*PI:#N],PI/2.*[1:1:#N]; sph );
_IBcirc.z += deltap;
_IBcirc = vector_rotate( _IBcirc, ey, i );
_IBcirc += struct_of_arrays_2_struct_array(_IB)[-1] - struct_of_arrays_2_struct_array(_IB)[0];
_IBcirc = struct_of_arrays_2_struct_array(_IBcirc);
%xp.shade_region( PP(_IBcirc) ; fillcolor=photon2,width=0);
xp.plot( PP(struct_of_arrays_2_struct_array(_IB)[-1]) ; sym="circle", color=photon2,fill, size=0.3*R);

% RHO
variable rhoc = 0.3*R*vector( [1:1:#N], PI/2+[0:PI/2-atan2(crho,srho):#N], PI/2*[1:1:#N] ; sph );
rhoc.z += deltap;
rhoc = vector_rotate( rhoc, ey, i );
xp.plot( PP(rhoc) ; line=0,color=obsplane );
xp.xylabel( PP(vector( mean(rhoc.x), mean(rhoc.y), mean(rhoc.z) )), "$\rho$"R, -.4, -.8;color=obsplane );

xp.plot( PP([R,deltap]*k) ; line=2, width=1 );

% inclination
variable ic = GC( ez, k );
xp.plot( PP(0.18*ic) );
xp.xylabel( PP(0.12*vector( mean(ic.x), mean(ic.y), mean(ic.z) )), "$i$"R );

% PSI
variable pc = GC( n, k );
xp.plot( PP(0.42*pc) ; color=photon1, depth=50);
xp.xylabel( PP(0.35*vector( mean(pc.x), mean(pc.y), mean(pc.z) )), "$\varPsi$"R, -.5, 0; color=photon1 );

variable _pc = GC( n, k ; R);
xp.plot( PP(0.33*_pc) ; color=photon2, depth=150 );
xp.xylabel( PP(1.*vector( mean(_pc.x), mean(_pc.y), mean(_pc.z) )), "$\varPsi^*$"R, -1.8, 0 ; color=photon2);

% Periastron
variable _per = _rp*vector_rotate( unit_vector(n), crossprod(k,n), _psi-_pp );
variable _pper = GC( _per, k);
xp.plot( PP([0,1]*_per) ; color=photon2 );
xp.xylabel( PP(0.6*_per), "$r_\mathrm{p}$"R, .7, .0 ; color=photon2);
xp.plot( PP(0.29*_pper) ; color=photon2, depth=150 );
xp.xylabel( PP(0.25*vector( mean(_pper.x), mean(_pper.y), mean(_pper.z) )), "$\varPsi_\mathrm{p}$"R, .25, .0 ; color=photon2);

%%% Emission point: R, n & help lines
xp.plot( PP([0,1]*R*n) ; line=1 );
xp.xylabel( PP(0.5*R*n), "$R$"R, .5, .5 );
xp.plot( PP([1,1.2*s]*R*n) );
xp.xylabel( PP(1.2*ls*R*n), "$\vec{n}$"R, -1,0 );
xp.plot( PP([1,1.2*s]*R*n); forward_arrow=ARROW );

xp.plot( PP(ncirc) ; line=2 );
xp.plot( PP(nline) ; line=2 );
xp.plot( PP(kncirc); line=1 );
xp.plot( PP(nkcirc); line=1 );

variable Scirc = vector( 0.05*[R:R:#N],[0:2*PI:#N],PI/2.*[1:1:#N]; sph );
Scirc.z += R;
Scirc = vector_rotate( Scirc, unit_vector(crossprod(ez,n)), theta );
Scirc = struct_of_arrays_2_struct_array(Scirc);
%xp.shade_region( PP(Scirc) ; fillcolor="black",width=0);
xp.plot( PP(R*n) ; sym="circle", fill, size=0.3*R, depth=40 );

% phi
variable phic = vector( 0.13*[R:R:#N], [0:phi:#N], [PI/2.:PI/2:#N]; sph );
xp.plot( PP(phic) );
xp.xylabel( PP(vector( mean(phic.x), mean(phic.y), mean(phic.z) )), "$\phi$"R, 1.2, -.1 );

% theta
variable tc = vector( 0.6*[R:R:#N], [phi:phi:#N], [0:theta:#N]; sph );
xp.plot( PP(tc) );
xp.xylabel( PP(0.8*vector( mean(tc.x), mean(tc.y), mean(tc.z) )), "$\theta$"R, -.1,-.5 );

% photon
xp.plot( PP(R*[n,n+(s-1)*k0]) ; line=0 , depth=40);
xp.xylabel( PP(R*(n+(ls-1)*k0)), "$\vec{k}_0$"R, 1.6, .6; depth=40 );
xp.plot( PP(R*[n,n+(s-1)*k0]); forward_arrow=ARROW, depth=40);

% alpha
variable ac = GC( k0, n );
xp.plot( PP(0.2*ac+R*n) );
xp.xylabel( PP(R*n+0.13*vector( mean(ac.x), mean(ac.y), mean(ac.z) )), "$\alpha$"R );

% trace
variable t1 = PT();
variable t1ind = where( vector_norm(t1) <= abs(vector(IB.x[-1],IB.y[-1],IB.z[-1])) );
xp.plot( PP(struct_filter( t1, t1ind ; copy ) ) ; color=photon1, depth=50, width=3 );
xp.plot( PP(struct_filter( t1, complement([0:length(t1ind)-1],t1ind) ; copy )); color=photon1, depth=30, line=1 );
variable t2 = _PT();
variable t2ind = where( vector_norm(t2) <= abs(vector(_IB.x[-1],_IB.y[-1],_IB.z[-1])) );
xp.plot( PP(struct_filter( t2, t2ind ; copy ) ) ; color=photon2, line=1,depth=250, width=3 );
xp.plot( PP(struct_filter( t2, complement([0:length(t2ind)-1],t2ind) ; copy ) ); color=photon2, depth=30, line=1 );

%%% FILL OBSERVER PLANE
variable fill1 = vector([kncirc.x,IB.x[[0,1]],struct_filter( t1, t1ind ; copy ).x],
[kncirc.y,IB.y[[0,1]],struct_filter( t1, t1ind ; copy ).y],
[kncirc.z,IB.z[[0,1]],struct_filter( t1, t1ind ; copy ).z]
);
variable _fill1 = vector([0,IB.x[[0,1]],struct_filter( t1, t1ind ; copy ).x],
[0,IB.y[[0,1]],struct_filter( t1, t1ind ; copy ).y],
[0,IB.z[[0,1]],struct_filter( t1, t1ind ; copy ).z]
);
variable fill2 = vector([nkcirc.x,_IB.x[[0,1]],struct_filter( t2, t2ind ; copy ).x],
[nkcirc.y,_IB.y[[0,1]],struct_filter( t2, t2ind ; copy ).y],
[nkcirc.z,_IB.z[[0,1]],struct_filter( t2, t2ind ; copy ).z]
);
variable _fill2 = vector([0,_IB.x[[0,1]],struct_filter( t2, t2ind ; copy ).x],
[0,_IB.y[[0,1]],struct_filter( t2, t2ind ; copy ).y],
[0,_IB.z[[0,1]],struct_filter( t2, t2ind ; copy ).z]
);
xp.shade_region( PP(_fill1); fillcolor=photon1, fill=36,depth=250, width=0 );
xp.shade_region( PP(_fill2); fillcolor=photon2, fill=36,depth=250, width=0 );

xp.render("geo.pdf");
xp.render("geo.png");

</pre>

Monsterlightcurve (xfig example)

2018-05-02T11:18:05Z

Sokolova-lapa: Created page with " Category:SLxfig File:monster_lightcurve_vg.png File ''common_pars.sl'', which I use to load some parameters common to all plots in a paper: <pre> %% -- set up vari..."

[[Category:SLxfig]]
[[File:monster_lightcurve_vg.png]]

File ''common_pars.sl'', which I use to load some parameters common to all plots in a paper:

<pre>
%% -- set up variables for plotting
variable width = 10;
variable height = 10;

variable fullwidth = 25;

variable mjdmin = MJDofDate(1995,12,15);
variable mjdmax = MJDofDate(2012,12,30);
variable yearmin = dateOfMJD(mjdmin);
variable yearmax = dateOfMJD(mjdmax);

variable max_asmh = 2.5;
variable min_asmh = 0.;
variable max_asmr = 150.;
variable min_asmr = 0.;

%%ends of activity periods
variable e1 = 50350;
variable e2 = 51000;
variable e3 = 53900;
variable e4 = 55375;

%%define colours
variable cl_hard = "blue";
variable cl_tran = "green4";
variable cl_soft = "red";
variable cl_neutral = "gray";

variable cl_hard_bg = "blue1";
variable cl_soft_bg = "pink3";

%%define data specific stuff
variable gamma_hard = 2.0;
variable gamma_soft = 2.5;

%define mapping parameters
variable asm_th = 20.; % threshold
variable asm_x0 = 0.28; %x-intersection
variable asm_hs = 55.; %hard slope
variable asm_ss = 350.; %soft slope

%%define paths to data
variable maxiname = "lc_1orbit-Cyg_X-1_55058.09375-56244.21875.csv"
</pre>

Actual plotting routine:

<pre>
require("isisscripts");
require("../common_pars");

variable width=25;
variable hh = 3.5;

variable asmmin = 0;
variable asmmax = 200;
variable asmamin = 0;
variable asmamax = 100;
variable asmcmin = 0;
variable asmcmax = 50;
variable batmin = -0.09;
variable batmax = 0.39;

variable asmarrow = 170;
variable ptext = 185;

variable dnd = fits_read_table("../data/all_disk_nodisk.fits");
variable obs = fits_read_table("../data/all_obs.fits");
variable tt = (obs.tstart+obs.tstop)/2.;
variable pca_hard = where(dnd.bknpower_1_phoindx1_value < gamma_hard);
variable pca_tran = where(gamma_hard <= dnd.bknpower_1_phoindx1_value < gamma_soft);
variable pca_soft = where(gamma_soft <= dnd.bknpower_1_phoindx1_value);

variable asm = RXTE_ASM_lightcurve("cygx1");
struct_filter(asm,where(asm.rate_a > 0));
struct_filter(asm,where(asm.rate_b > 0));
struct_filter(asm,where(asm.rate_c > 0));

variable asm_late = struct_filter(asm,where(asm.time > 55200);copy,dim=0);
struct_filter(asm,where(asm.time < 55200));

variable hardness = asm.rate_c/asm.rate_a;

variable asm_hard = where(asm.rate <= asm_th or asm.rate <= (hardness-asm_x0)*asm_hs);
variable asm_tran = where(asm.rate > asm_th and asm.rate > (hardness-asm_x0)*asm_hs
and asm.rate <= (hardness-asm_x0)*asm_ss);
variable asm_soft = where(asm.rate > asm_th and asm.rate > (hardness-asm_x0)*asm_ss);

%%index for the times during the longhard state
variable ind_longhard = where( 53900 < asm.time < 54900);

%BAT
variable bat = fits_read_table("../data/CygX-1.orbit.lc.fits"); %
bat.time = bat.time/3600./24.+51910+0.00074287038;

struct_filter(bat,where(bat.time < 56240));

variable bat_soft = where(bat.rate <= 0.09);
variable bat_uncat = where(bat.rate > 0.09);

%%MAXI
variable maxi = ascii_read_table("../data/"+maxiname,
[{"%F","time"},{"%F","rate"},{"%F","err"},
{"%F","lo"},{"%F","loerr"},
{"%F","mi"},{"%F","mierr"},
{"%F","hi"},{"%F","hierr"}]);

struct_filter(maxi,where(maxi.time < 56240));

variable maxi_hard = where(maxi.lo <= 1.4*maxi.mi/maxi.lo);
variable maxi_tran = where(1.4*maxi.mi/maxi.lo < maxi.lo <= 8./3.*maxi.mi/maxi.lo);
variable maxi_soft = where(maxi.lo > 8./3.*maxi.mi/maxi.lo);

%%GBM
()=evalfile("../gbm/init_gbm.sl");
variable gbm = @d;
%struct_filter(gbm, where(gbm.nr_occ>10));
struct_filter(gbm,where(gbm.mjd_start < 56240));
variable gbm_soft = where(1e-3*get_struct_field (gbm, cnfg.flux[1]) < 0.6);
variable gbm_uncat = where(1e-3*get_struct_field (gbm, cnfg.flux[1]) > 0.6);

%%axis labels
variable mino = [1996:2013];
variable maj = [1996:2013]+0.5;
variable extramin = Double_Type[0];
variable q,i;
variable ticc=String_Type[length(maj)];
_for i (0,2013-1996-1,1){
ticc[i]=string(mino[i]);
_for q (1,11,1){
extramin = [extramin,1996+i+q/12.];
}
}

variable plg = xfig_plot_new(width,hh*5./7.);
plg.world1(mjdmin,mjdmax,-1,4);
plg.world2(yearmin.year+(yearmin.month-1)/12.+yearmin.day/365.,
yearmax.year+(yearmax.month-1)/12.+yearmax.day/365.,
-1,4);
plg.x1axis(;off);
plg.x2axis(;major = maj, minor = mino, ticlabels = ticc,
major_len=0,minor_len=0.2,minor_width=2
);
plg.yaxis(;ticlabels=0,major=0,minor=0);
_for i (0,length(pca_hard)-1,1){
plg.plot([tt[pca_hard[i]],tt[pca_hard[i]]],[2,3];color=cl_hard);
};
_for i (0,length(pca_tran)-1,1){
plg.plot([tt[pca_tran[i]],tt[pca_tran[i]]],[1,2];color=cl_tran);
};
_for i (0,length(pca_soft)-1,1){
plg.plot([tt[pca_soft[i]],tt[pca_soft[i]]],[0,1];color=cl_soft);
};
plg.ylabel("\begin{center}times of\\pointed \\\textsl{RXTE} obs.\end{center}"R;rotate=-90);
plg.x2label("year");

variable pl_asm = xfig_plot_new(width,hh);
pl_asm.world1(mjdmin,mjdmax,asmmin,asmmax);
pl_asm.world2(yearmin.year+(yearmin.month-1)/12.+yearmin.day/365.,
yearmax.year+(yearmax.month-1)/12.+yearmax.day/365.,
asmmin,asmmax);
pl_asm.x2axis(;off);
pl_asm.y2axis(;ticlabels=0);
pl_asm.plot(asm.time[asm_tran],asm.rate[asm_tran];sym="point",size=0.1,color=cl_tran);
pl_asm.plot(asm.time[asm_soft],asm.rate[asm_soft];sym="point",size=0.1,color=cl_soft);
pl_asm.plot(asm.time[asm_hard],asm.rate[asm_hard];sym="point",size=0.1,color=cl_hard);
pl_asm.plot(asm_late.time,asm_late.rate;sym="point",size=0.1,color="gray");
pl_asm.plot([e1,e1],[asmmin,asmmax];line=1,width=2,depth=10);
pl_asm.plot([e2,e2],[asmmin,asmmax];line=1,width=2,depth=10);
pl_asm.plot([e3,e3],[asmmin,asmmax];line=1,width=2,depth=10);
pl_asm.plot([e4,e4],[asmmin,asmmax];line=1,width=2,depth=10);
pl_asm.plot([mjdmin,e1],[asmarrow,asmarrow];
line=0, forward_arrow, arrow_thickness =1,color="gray");
pl_asm.plot([e1,e2],[asmarrow,asmarrow];
line=0, forward_arrow, backward_arrow, arrow_thickness =1,color="gray");
pl_asm.plot([e2,e3],[asmarrow,asmarrow];
line=0, forward_arrow, backward_arrow, arrow_thickness =1,color="gray");
pl_asm.plot([e3,e4],[asmarrow,asmarrow];
line=0, forward_arrow, backward_arrow, arrow_thickness =1,color="gray");
pl_asm.plot([e4,mjdmax],[asmarrow,asmarrow];
line=0, backward_arrow, arrow_thickness =1,color="gray");
pl_asm.xylabel((mjdmin+e1)/2.,ptext,"I";depth=10);
pl_asm.xylabel((e1+e2)/2.,ptext,"II";depth=10);
pl_asm.xylabel((e2+e3)/2.,ptext,"period III";depth=10);
pl_asm.xylabel((e3+e4)/2.,ptext,"period IV";depth=10);
pl_asm.xylabel((e4+mjdmax)/2.,ptext,"period V";depth=10);
pl_asm.ylabel("\begin{center}\textsl{RXTE}-ASM \\1.5--12\,keV \\$[$cps$]$\end{center}"R);

variable pl_asmh = xfig_plot_new(width,hh);
pl_asmh.world1(mjdmin,mjdmax,0.08,15;ylog);
pl_asmh.world2(yearmin.year+(yearmin.month-1)/12.+yearmin.day/365.,
yearmax.year+(yearmax.month-1)/12.+yearmax.day/365.,
0.08,10;ylog);
pl_asmh.x2axis(;major = maj, minor = mino, ticlabels = ticc,
major_len=0,minor_len=0.2,minor_width=2
);
pl_asmh.y2axis(;ticlabels=0);
%pl_asmh.y1axis(;format="$10^{%.1f}$"R);
pl_asmh.plot(asm.time[asm_tran],asm.rate_c[asm_tran]/asm.rate_a[asm_tran];
sym="point",size=0.1,color=cl_tran);
pl_asmh.plot(asm.time[asm_soft],asm.rate_c[asm_soft]/asm.rate_a[asm_soft];
sym="point",size=0.1,color=cl_soft);
pl_asmh.plot(asm.time[asm_hard],asm.rate_c[asm_hard]/asm.rate_a[asm_hard];
sym="point",size=0.1,color=cl_hard);
pl_asmh.plot(asm_late.time,asm_late.rate_c/asm_late.rate_a;
sym="point",size=0.1,color="gray");
pl_asmh.plot([e1,e1],[asmmin,asmmax];line=1,width=2,depth=10);
pl_asmh.plot([e2,e2],[asmmin,asmmax];line=1,width=2,depth=10);
pl_asmh.plot([e3,e3],[asmmin,asmmax];line=1,width=2,depth=10);
pl_asmh.plot([e4,e4],[asmmin,asmmax];line=1,width=2,depth=10);
pl_asmh.ylabel("\begin{center}\textsl{RXTE}-ASM \\ hardness \\ (C$/$A)\end{center}"R);

variable pl_bat = xfig_plot_new(width,hh);
pl_bat.world(mjdmin,mjdmax,batmin,batmax);
pl_bat.world2(yearmin.year+(yearmin.month-1)/12.+yearmin.day/365.,
yearmax.year+(yearmax.month-1)/12.+yearmax.day/365.,batmin,batmax);
pl_bat.y2axis(;ticlabels=0,tic_depth=3);
pl_bat.x2axis(;major = maj, minor = mino, ticlabels = ticc,
major_len=0,minor_len=0.2,minor_width=2
);
pl_bat.plot(bat.time[bat_soft],bat.rate[bat_soft];sym="point",size=0.1,color=cl_soft);
pl_bat.plot(bat.time[bat_uncat],bat.rate[bat_uncat];sym="point",size=0.1);
pl_bat.plot([e1,e1],[batmin,batmax];line=1,width=2,depth=10);
pl_bat.plot([e2,e2],[batmin,batmax];line=1,width=2,depth=10);
pl_bat.plot([e3,e3],[batmin,batmax];line=1,width=2,depth=10);
pl_bat.plot([e4,e4],[batmin,batmax];line=1,width=2,depth=10);
pl_bat.plot([mjdmin,mjdmax],[0,0];color="gray",line=1);
pl_bat.y1axis(;format="%.1f",tic_depth=3);
pl_bat.ylabel("\begin{center}\textsl{Swift}-BAT \\ 15--50\,keV \\$[$cps/cm$^2]$\end{center}"R);

variable pl_maxi = xfig_plot_new(width,hh);
pl_maxi.world(mjdmin,mjdmax,0,5.5);
pl_maxi.world2(yearmin.year+(yearmin.month-1)/12.+yearmin.day/365.,
yearmax.year+(yearmax.month-1)/12.+yearmax.day/365.,0,6);
pl_maxi.x2axis(;major = maj, minor = mino, ticlabels = ticc,
major_len=0,minor_len=0.2,minor_width=2
);
pl_maxi.y2axis(;ticlabels=0);
pl_maxi.plot(maxi.time[maxi_tran],maxi.rate[maxi_tran];sym="point",size=0.1,color=cl_tran);
pl_maxi.plot(maxi.time[maxi_soft],maxi.rate[maxi_soft];sym="point",size=0.1,color=cl_soft);
pl_maxi.plot(maxi.time[maxi_hard],maxi.rate[maxi_hard];sym="point",size=0.1,color=cl_hard);
pl_maxi.plot([e1,e1],[0,6];line=1,width=2,depth=10);
pl_maxi.plot([e2,e2],[0,6];line=1,width=2,depth=10);
pl_maxi.plot([e3,e3],[0,6];line=1,width=2,depth=10);
pl_maxi.plot([e4,e4],[0,6];line=1,width=2,depth=10);
pl_maxi.ylabel("\begin{center}MAXI \\ 2--20\,keV \\$[$cps/cm$^2]$\end{center}"R);

variable pl_gbm = xfig_plot_new(width,hh);
pl_gbm.world(mjdmin,mjdmax,-0.4,1.9);
pl_gbm.world2(yearmin.year+(yearmin.month-1)/12.+yearmin.day/365.,
yearmax.year+(yearmax.month-1)/12.+yearmax.day/365.,-0.4,1.9);
pl_gbm.x2axis(;major = maj, minor = mino, ticlabels = ticc,
major_len=0,minor_len=0.2,minor_width=2
);
pl_gbm.y1axis(;format="%.1f",tic_depth=3);
pl_gbm.y2axis(;ticlabels=0,tic_depth=3);
pl_gbm.plot(0.5*(gbm.mjd_start + gbm.mjd_stop)[gbm_soft],
1e-3*get_struct_field (gbm, cnfg.flux[1])[gbm_soft],
0.5* (gbm.mjd_stop - gbm.mjd_start)[gbm_soft],
1e-3*get_struct_field (gbm, cnfg.err[1])[gbm_soft];
sym = "point",color=cl_soft);
pl_gbm.plot(0.5*(gbm.mjd_start + gbm.mjd_stop)[gbm_uncat],
1e-3*get_struct_field (gbm, cnfg.flux[1])[gbm_uncat],
0.5* (gbm.mjd_stop - gbm.mjd_start)[gbm_uncat],
1e-3*get_struct_field (gbm, cnfg.err[1])[gbm_uncat];
sym = "point");
pl_gbm.plot([mjdmin,mjdmax],[0,0];color="gray",line=1);
pl_gbm.plot([e1,e1],[-0.4,1.9];line=1,width=2,depth=10);
pl_gbm.plot([e2,e2],[-0.4,1.9];line=1,width=2,depth=10);
pl_gbm.plot([e3,e3],[-0.4,1.9];line=1,width=2,depth=10);
pl_gbm.plot([e4,e4],[-0.4,1.9];line=1,width=2,depth=10);
pl_gbm.ylabel("\begin{center}GBM \\ 25--50\,keV \\ $[$Crab$]$\end{center}"R);

variable comp = xfig_new_vbox_compound(plg,
xfig_multiplot(pl_asm,pl_asmh,
pl_maxi,
pl_bat,pl_gbm;
xlabel="MJD"));
comp.render("monster.pdf");

print("STACK:");
_print_stack;
exit;
</pre>

Model decomp (xfig example)

2018-05-02T11:16:18Z

Sokolova-lapa: Created page with " Category:SLxfig File:multipanel_decomposition.png Spectral data and models of the best fits have been stored in tables using write_plot() and eval_fun_keV() in a..."

[[Category:SLxfig]]

[[File:multipanel_decomposition.png]]

Spectral data and models of the best fits have been stored in tables using write_plot() and eval_fun_keV() in a file structure of shape /userdata/data/user/ "source" / "model" /decomposition/ "component"

<pre>
#!/usr/bin/env isis-script

require("isisscripts");

variable COLOR = ["dimgray","darkgray","lightgrey"];
variable MCOLOR = ["darkorange","blue","mediumaquamarine","purple","black"];

% Lists of object names and model components to automatically build data paths
variable comp_list = {"tbnew_feo*relxilllp","tbnew_feo*powerlaw","tbnew_feo*xillver","complete_model","absorbed_model"};
variable namelist = {"ark120","pds456","fairall9", "ngc1365", "3c390_3", "3c382"};
variable tex_name = {"Ark 120","PDS 456","Fairall 9", "NGC 1365", "3C390.3", "3C382"};
variable detconst = {{1,1/1.08,1/1.1},{1,1/0.68,1/0.75},{1,1/0.995,1/1.02},{1,1/0.96,1/0.98},{1,1/1.062567,1/1.115621},{1,1/0.8153,1/0.7853389}};

%-------main-loop-over-namelist---------------
variable panel = Struct_Type[length(namelist)];
variable i,j, lo, hi, val, err, err_max, err_min;

for(j=0;j<length(namelist);j++){

% initialize panel j
panel[j] = xfig_plot_new(12, 9);
panel[j].world(0.5,80,5e-08,0.1; xlog=1, ylog=1);
panel[j].ylabel(`Flux \footnotesize[s$^{-1}$\,cm$^{-2}$\,keV$^{-1}$]`);
panel[j].xylabel(0.95,0.9,tex_name[j],0.5,0; world0);

variable write_folder = "/userdata/data/fink/"+namelist[j]+"/fit_relxilllp/decomposition/";

% plot data from three detectors in the background, corrected for according detector constant
for(i=0;i<=2;i++){
(lo, hi, val, err) = readcol(write_folder+"data_"+string(i)+".dat", 1, 2, 3, 4);
panel[j].plot((lo+hi)/2., val*detconst[j][i], err*detconst[j][i]; sym="point", size=-1, eb_factor=0, color=COLOR[i]);
}

% plot model components (exception for pds456)
for(i=0;i<length(comp_list);i++){
if(not(comp_list[i]=="tbnew_feo*xillver" && namelist[j] == "pds456")){
(lo, hi, val) = readcol(write_folder+comp_list[i]+".dat", 1, 2, 3);
panel[j].plot((lo+hi)/2, val; line=0, eb_factor=0, size=0.01, color=MCOLOR[i], depth=10-i);
}
}
}

% some model labels
variable ypos = 0.42, ystep = 0.08;
panel[1].xylabel(0.05, ypos - 0*ystep, "Powerlaw", -0.5, 0; world0, color = MCOLOR[1]);
panel[1].xylabel(0.05, ypos - 1*ystep, "CDR",-0.5,0; world0, color = MCOLOR[2]);
panel[1].xylabel(0.05, ypos - 2*ystep, "Lamppost-RR",-0.5,0; world0, color = MCOLOR[0]);
panel[1].xylabel(0.05, ypos - 3*ystep, "Powerlaw + Reflection",-0.5,0; world0, color = MCOLOR[3]);
panel[1].xylabel(0.05, ypos - 4*ystep, "Full Absorbed Model",-0.5,0; world0, color = MCOLOR[4]);

%---------render-all--------------
variable multi = xfig_multiplot(panel; xlabel=`Energy [keV]`, cols=2);
multi.render("multipanel_decomposition.pdf");

quit;
</pre>

Compounds and multi-panel plots (xfig example)

2018-04-13T16:55:26Z

Sokolova-lapa: Created page with " Category:SLxfig an example added by Manfred ===== Compounds ===== A 'compound' is a collection of several Xfig objects (of any type) that are grouped toge..."

[[Category:SLxfig]]
an example added by Manfred

===== Compounds =====
A 'compound' is a collection of several Xfig objects (of any type) that are grouped together,
i.e., they can be rendered at once and be transformed – e.g., translated, scaled, and maybe rotated – together.

The function <code>xfig_new_compound</code> creates such a 'compound' as an SLxfig object, see
help("xfig_new_compound");
Note that <code>xfig_new_compound</code> assumes that the member objects are already aligned with respect to each other.

In contrast, the functions <code>xfig_new_hbox_compound</code> and <code>xfig_new_vbox_compound</code>
translate the objects (which are given as arguments to these functions) in horizontal, respectively vertical direction
such that those become aligned next to, respectively on top of each other.
Additional spacing can be specified as an optional last argument.

While <code>xfig_multiplot</code> can take an array of plots like <code>xfig_multiplot([pl1,pl2,pl3])</code>, <code>xfig_new_*compound</code> needs each plot to be an individual argument: <code>xfig_new_*compound(pl1,pl2,pl3)</code>. The use of <code>_ _push_array</code> (available through the isisscripts) helps to circumvent this issue:
<code>
require("isisscripts");
...
variable plotlist = [pl1,pl2,pl3];
...
xfig_new_hbox_compound(__array_push(plotlist));
</code>
===== Multi-panel plots =====
The function <code>xfig_multiplot</code> combines several plot objects
(which are themselves compounds of many low-level objects, such as lines and images)
into a compound object, and additionally removes those labels and ticlabels
that are superfluous if more plots share the same axes.
However, the user must ensure him/herself that the plots which are to be combined in a multiplot,
have all the same respective axes!

===== Example =====
variable W=5, H=4, % width & height; all plots will use these sizes
x=[-sqrt(2):sqrt(2):#101]; % and these values on the x-axis

variable pl11=xfig_plot_new(W, H);
pl11.plot(x,x^4);

variable pl12=xfig_plot_new(W, H);
pl12.plot(x, -x^2);

variable pl2=xfig_plot_new(W, 2*H); % twice as high
pl2.plot(x, x^4-x^2);

% combine plots pl11 and pl12 to a mulitplot
variable mp1 = xfig_multiplot(pl11, pl12);

% combine the multiplot mp1 and the plot pl2 horizontally next to each other
variable comp = xfig_new_hbox_compound(mp1, pl2, 0.3);
comp.render("multiplot_and_plot.eps");
[[File:multiplot_and_plot.png|multiplot_and_plot.png]]

If <code>mp1</code> and <code>comp</code> are not needed for anything else, the latter three commands could also have been combined into a single one:
xfig_new_hbox_compound( xfig_multiplot(pl11, pl12),
pl2,
0.3
).render("multiplot_and_plot.eps");

Note that for the creation of the above image, I took advantage of <code>comp</code> being a compound, and resized all objects together:
comb.scale(0.75);
comp.render("multiplot_and_plot.png");

Two-dimensional histograms (xfig example)

2018-04-13T16:45:21Z

Sokolova-lapa:

[[Category:SLxfig]]
example added by Manfred

Similarly to the [[Example: color-coded maps with 2d histograms, png, and xfig|first example]] for creating [[Example: color-coded maps with 2d histograms, png, and xfig|color-coded maps]] with the [[Plotting_with_the_S-Lang_Xfig_module|SLxfig module]], the goal of this one is to produce a color-coded map,
but this time, the color-scale represents a density of (a possibly large number of) data points.

=== ISIS' histogram2d function ===

==== Usage ====
The <code>histogram2d</code> function is used in the following way (see also [http://pulsar.sternwarte.uni-erlangen.de/hanke/science/X-ray/ISIS/cgi/help.cgi?subj=histogram2d help("histogram2d")]):
num = histogram2d(A, B, Agrid, Bgrid);
<code>A</code> and <code>B</code> have to be <code>Double_Type</code> arrays of the same length,
<code>Agrid</code> and <code>Bgrid</code> have to be <code>Double_Type</code> arrays with monotonically increasing elements.

Now, <code>num[a,b]</code> contains the number of points (<code>A</code>, <code>B</code>)
falling into each 2d-bin defined by the lower bin boundaries <code>Agrid[a]</code> and <code>Bgrid[b]</code>, i.e.:
num[a,b] == howmany( (Agrid[a] <= A < Agrid[a+1]) and (Bgrid[b] <= B < Bgrid[b+1]) );

==== Overflow bins ====
The last bin in each row or column is an overflow bin whose upper limit is at infinity, i.e.,
num[-1,b] == howmany( (Agrid[-1] <= A) and (Bgrid[b] <= B < Bgrid[b+1]) );
num[a,-1] == howmany( (Agrid[a] <= A < Agrid[a+1]) and (Bgrid[-1] <= B) );
and
num[-1,-1] == howmany( (Agrid[-1] <= A) and (Bgrid[-1] <= B) );

If one wants to remove these overflow bins,
one can simply apply the index-array <code>[:-2]</code> (which means "take all elements up to the second last one")
in both dimensions in order to create a smaller two-dimensional array:
num_ = num[ [:-2], [:-2] ];

The last bins corresponding to the reduced 2d-array <code>num_</code> end now at the same position where the grids end, too:
num_[-1,-1] == num[-2,-2] == howmany( (Agrid[-2] <= A < Agrid[-1]) and (Bgrid[-2] <= B < Bgrid[-1]) );
Before, the grids specified always lower bin boundaries,
but now, the grids have one element more than the correpsonding array-dimensions of <code>num_</code>.

Note that ISIS (one-dimensional) <code>histogram</code> function does not produce an overflow bin.

==== Order of the indices ====
The first index of <code>num</code> (called <code>a</code> above) will always correspond
to the first [and third] argument of the <code>histogram2d</code> function (here called <code>A</code> [and <code>Agrid</code>]),
and the second index (<code>b</code>) to the second [and fourth] argument (<code>B</code> [and <code>Bgrid</code>]).

As most functions that operate on two dimensional arrays (like <code>plot_image</code>, <code>png_write</code>, <code>ds9_view</code>, ...)
expect that the first index of the 2d-array to correspond to the y-axis,
whereas only the second index to the x-axis,
one will have to pass the y-data [and -grid] before the x-data [and -grid]:
num = histogram2d(Y, X, Xgrid, Ygrid);

=== Using two-dimensional histograms ===

Just as in the [[Example:_color-coded_maps_with_2d_histograms,_png,_and_xfig|previous example]],
these two dimensional histograms can be transformed into a color-coded image,
which can then be included in an [[Plotting_with_the_S-Lang_Xfig_module|xfig plot]] which adds back the original coordinate system.

==== A "banana-plot" ====

In an X-ray gratings spectrometer (Chandra-HETGS, XMM-RGS),
the dispersion is not only proportional to the photon's wavelength, but also to the dispersion order.
Different orders, however, can be separated with the internal energy resolution of the CCD detector.

The following example plots the density of events in a position – energy diagram:

===== Writing the png image =====

<pre>
variable evts = fits_read_table("evt2.fits"); % reading a Chandra level-2 event file

variable x_grid = [2300:5700:#320]; % x position on the detector (320 values)
variable energy_grid = [0:10000:#240]; % energies in eV (240 values from 0 to 10 keV)

variable num = histogram2d(evts.energy, evts.x, % the data (Y, X)
energy_grid, x_grid % the grids (Ygrid, Xgrid)
)[[:-2],[:-2]]; % removing overflow bins

require("png"); % load png module
variable RGB = png_gray_to_rgb(log(1+num), "ds9sls"); % transform num values logarithmically to RGB values, using the ds9sls color map
png_write_flipped("banana.png", RGB); % write RGB values to a png file
% png_write_flipped places RGB[0,0] in the *lower* left corner
</pre>
This produces just the bare image "banana.png":

[[File:banana.png|bare image "banana.png"]]

With the [[Plotting_with_the_S-Lang_Xfig_module|S-Lang xfig module]], the coordinate system can, however, be easily added (back again).

===== Plotting the png into an SLxfig plot =====

It is important to set the correct coordinates for the SLxfig plot object,
as this information is no more present in the bare image.
As discussed above (in the section on "overflow bins"),
the last bins of the reduced 2d-array end where the original grids end
– and obviously the first bins start where the grids start.
This is all the information that needs to be passed to the <code>world</code> method of an SLxfig plot object:
<pre>
require("xfig");
variable p = xfig_plot_new();
p.world(x_grid[0], x_grid[-1], energy_grid[0]/1000, energy_grid[-1]/1000); % defining the coordinate system; energy in keV instead of eV
p.plot_png("banana.png");
p.xlabel("Sky X Position");
p.ylabel("Energy [keV]");
p.render("banana-plot.pdf");
</pre>
The resulting plot looks like this:

[[File:banana-plot.png|banana-plot with coordinate system]]

Two-dimensional histograms (xfig example)

2018-04-13T14:13:09Z

Sokolova-lapa:

[[Category:SLxfig]]
example added by Manfred

Similarly to the [[Example: color-coded maps with 2d histograms, png, and xfig|first example]] for creating [[Example: color-coded maps with 2d histograms, png, and xfig|color-coded maps]] with the [[Plotting_with_the_S-Lang_Xfig_module|SLxfig module]], the goal of this one is to produce a color-coded map,
but this time, the color-scale represents a density of (a possibly large number of) data points.

=== ISIS' histogram2d function ===

==== Usage ====
The <code>histogram2d</code> function is used in the following way (see also [http://pulsar.sternwarte.uni-erlangen.de/hanke/science/X-ray/ISIS/cgi/help.cgi?subj=histogram2d help("histogram2d")]):
num = histogram2d(A, B, Agrid, Bgrid);
<code>A</code> and <code>B</code> have to be <code>Double_Type</code> arrays of the same length,
<code>Agrid</code> and <code>Bgrid</code> have to be <code>Double_Type</code> arrays with monotonically increasing elements.

Now, <code>num[a,b]</code> contains the number of points (<code>A</code>, <code>B</code>)
falling into each 2d-bin defined by the lower bin boundaries <code>Agrid[a]</code> and <code>Bgrid[b]</code>, i.e.:
num[a,b] == howmany( (Agrid[a] <= A < Agrid[a+1]) and (Bgrid[b] <= B < Bgrid[b+1]) );

==== Overflow bins ====
The last bin in each row or column is an overflow bin whose upper limit is at infinity, i.e.,
num[-1,b] == howmany( (Agrid[-1] <= A) and (Bgrid[b] <= B < Bgrid[b+1]) );
num[a,-1] == howmany( (Agrid[a] <= A < Agrid[a+1]) and (Bgrid[-1] <= B) );
and
num[-1,-1] == howmany( (Agrid[-1] <= A) and (Bgrid[-1] <= B) );

If one wants to remove these overflow bins,
one can simply apply the index-array <code>[:-2]</code> (which means "take all elements up to the second last one")
in both dimensions in order to create a smaller two-dimensional array:
num_ = num[ [:-2], [:-2] ];

The last bins corresponding to the reduced 2d-array <code>num_</code> end now at the same position where the grids end, too:
num_[-1,-1] == num[-2,-2] == howmany( (Agrid[-2] <= A < Agrid[-1]) and (Bgrid[-2] <= B < Bgrid[-1]) );
Before, the grids specified always lower bin boundaries,
but now, the grids have one element more than the correpsonding array-dimensions of <code>num_</code>.

Note that ISIS (one-dimensional) <code>histogram</code> function does not produce an overflow bin.

==== Order of the indices ====
The first index of <code>num</code> (called <code>a</code> above) will always correspond
to the first [and third] argument of the <code>histogram2d</code> function (here called <code>A</code> [and <code>Agrid</code>]),
and the second index (<code>b</code>) to the second [and fourth] argument (<code>B</code> [and <code>Bgrid</code>]).

As most functions that operate on two dimensional arrays (like <code>plot_image</code>, <code>png_write</code>, <code>ds9_view</code>, ...)
expect that the first index of the 2d-array to correspond to the y-axis,
whereas only the second index to the x-axis,
one will have to pass the y-data [and -grid] before the x-data [and -grid]:
num = histogram2d(Y, X, Xgrid, Ygrid);

=== Using two-dimensional histograms ===

Just as in the [[Example:_color-coded_maps_with_2d_histograms,_png,_and_xfig|previous example]],
these two dimensional histograms can be transformed into a color-coded image,
which can then be included in an [[Plotting_with_the_S-Lang_Xfig_module|xfig plot]] which adds back the original coordinate system.

==== A "banana-plot" ====

In an X-ray gratings spectrometer (Chandra-HETGS, XMM-RGS),
the dispersion is not only proportional to the photon's wavelength, but also to the dispersion order.
Different orders, however, can be separated with the internal energy resolution of the CCD detector.

The following example plots the density of events in a position &dash energy diagram:

===== Writing the png image =====

<pre>
variable evts = fits_read_table("evt2.fits"); % reading a Chandra level-2 event file

variable x_grid = [2300:5700:#320]; % x position on the detector (320 values)
variable energy_grid = [0:10000:#240]; % energies in eV (240 values from 0 to 10 keV)

variable num = histogram2d(evts.energy, evts.x, % the data (Y, X)
energy_grid, x_grid % the grids (Ygrid, Xgrid)
)[[:-2],[:-2]]; % removing overflow bins

require("png"); % load png module
variable RGB = png_gray_to_rgb(log(1+num), "ds9sls"); % transform num values logarithmically to RGB values, using the ds9sls color map
png_write_flipped("banana.png", RGB); % write RGB values to a png file
% png_write_flipped places RGB[0,0] in the *lower* left corner
</pre>
This produces just the bare image "banana.png":

[[File:banana.png|bare image "banana.png"]]

With the [[Plotting_with_the_S-Lang_Xfig_module|S-Lang xfig module]], the coordinate system can, however, be easily added (back again).

===== Plotting the png into an SLxfig plot =====

It is important to set the correct coordinates for the SLxfig plot object,
as this information is no more present in the bare image.
As discussed above (in the section on "overflow bins"),
the last bins of the reduced 2d-array end where the original grids end
&ndash and obviously the first bins start where the grids start.
This is all the information that needs to be passed to the <code>world</code> method of an SLxfig plot object:
<pre>
require("xfig");
variable p = xfig_plot_new();
p.world(x_grid[0], x_grid[-1], energy_grid[0]/1000, energy_grid[-1]/1000); % defining the coordinate system; energy in keV instead of eV
p.plot_png("banana.png");
p.xlabel("Sky X Position");
p.ylabel("Energy [keV]");
p.render("banana-plot.pdf");
</pre>
The resulting plot looks like this:

[[File:banana-plot.png|banana-plot with coordinate system]]

Two-dimensional histograms (xfig example)

2018-04-13T13:34:11Z

Sokolova-lapa:

[[Category:SLxfig]]
example added by Manfred

Similarly to the [[Example: color-coded maps with 2d histograms, png, and xfig|first example]] for creating [[Example: color-coded maps with 2d histograms, png, and xfig|color-coded maps]] with the [[Plotting_with_the_S-Lang_Xfig_module|SLxfig module]], the goal of this one is to produce a color-coded map,
but this time, the color-scale represents a density of (a possibly large number of) data points.

=== ISIS' histogram2d function ===

==== Usage ====
The <code>histogram2d</code> function is used in the following way (see also [http://pulsar.sternwarte.uni-erlangen.de/hanke/science/X-ray/ISIS/cgi/help.cgi?subj=histogram2d help("histogram2d")]):
num = histogram2d(A, B, Agrid, Bgrid);
<code>A</code> and <code>B</code> have to be <code>Double_Type</code> arrays of the same length,
<code>Agrid</code> and <code>Bgrid</code> have to be <code>Double_Type</code> arrays with monotonically increasing elements.

Now, <code>num[a,b]</code> contains the number of points (<code>A</code>, <code>B</code>)
falling into each 2d-bin defined by the lower bin boundaries <code>Agrid[a]</code> and <code>Bgrid[b]</code>, i.e.:
num[a,b] == howmany( (Agrid[a] <= A < Agrid[a+1]) and (Bgrid[b] <= B < Bgrid[b+1]) );

==== Overflow bins ====
The last bin in each row or column is an overflow bin whose upper limit is at infinity, i.e.,
num[-1,b] == howmany( (Agrid[-1] <= A) and (Bgrid[b] <= B < Bgrid[b+1]) );
num[a,-1] == howmany( (Agrid[a] <= A < Agrid[a+1]) and (Bgrid[-1] <= B) );
and
num[-1,-1] == howmany( (Agrid[-1] <= A) and (Bgrid[-1] <= B) );

If one wants to remove these overflow bins,
one can simply apply the index-array <code>[:-2]</code> (which means "take all elements up to the second last one")
in both dimensions in order to create a smaller two-dimensional array:
num_ = num[ [:-2], [:-2] ];

The last bins corresponding to the reduced 2d-array <code>num_</code> end now at the same position where the grids end, too:
num_[-1,-1] == num[-2,-2] == howmany( (Agrid[-2] <= A < Agrid[-1]) and (Bgrid[-2] <= B < Bgrid[-1]) );
Before, the grids specified always lower bin boundaries,
but now, the grids have one element more than the correpsonding array-dimensions of <code>num_</code>.

Note that ISIS (one-dimensional) <code>histogram</code> function does not produce an overflow bin.

==== Order of the indices ====
The first index of <code>num</code> (called <code>a</code> above) will always correspond
to the first [and third] argument of the <code>histogram2d</code> function (here called <code>A</code> [and <code>Agrid</code>]),
and the second index (<code>b</code>) to the second [and fourth] argument (<code>B</code> [and <code>Bgrid</code>]).

As most functions that operate on two dimensional arrays (like <code>plot_image</code>, <code>png_write</code>, <code>ds9_view</code>, ...)
expect that the first index of the 2d-array to correspond to the y-axis,
whereas only the second index to the x-axis,
one will have to pass the y-data [and -grid] before the x-data [and -grid]:
num = histogram2d(Y, X, Xgrid, Ygrid);

=== Using two-dimensional histograms ===

Just as in the [[Example:_color-coded_maps_with_2d_histograms,_png,_and_xfig|previous example]],
these two dimensional histograms can be transformed into a color-coded image,
which can then be included in an [[Plotting_with_the_S-Lang_Xfig_module|xfig plot]] which adds back the original coordinate system.

==== A "banana-plot" ====

In an X-ray gratings spectrometer (Chandra-HETGS, XMM-RGS),
the dispersion is not only proportional to the photon's wavelength, but also to the dispersion order.
Different orders, however, can be separated with the internal energy resolution of the CCD detector.

The following example plots the density of events in a position - energy diagram:

===== Writing the png image =====

<pre>
variable evts = fits_read_table("evt2.fits"); % reading a Chandra level-2 event file

variable x_grid = [2300:5700:#320]; % x position on the detector (320 values)
variable energy_grid = [0:10000:#240]; % energies in eV (240 values from 0 to 10 keV)

variable num = histogram2d(evts.energy, evts.x, % the data (Y, X)
energy_grid, x_grid % the grids (Ygrid, Xgrid)
)[[:-2],[:-2]]; % removing overflow bins

require("png"); % load png module
variable RGB = png_gray_to_rgb(log(1+num), "ds9sls"); % transform num values logarithmically to RGB values, using the ds9sls color map
png_write_flipped("banana.png", RGB); % write RGB values to a png file
% png_write_flipped places RGB[0,0] in the *lower* left corner
</pre>
This produces just the bare image "banana.png":

{{:isis:slxfig:banana.png|bare image "banana.png"}}

With the [[Plotting_with_the_S-Lang_Xfig_module|S-Lang xfig module]], the coordinate system can, however, be easily added (back again).

===== Plotting the png into an SLxfig plot =====

It is important to set the correct coordinates for the SLxfig plot object,
as this information is no more present in the bare image.
As discussed above (in the section on "overflow bins"),
the last bins of the reduced 2d-array end where the original grids end
-- and obviously the first bins start where the grids start.
This is all the information that needs to be passed to the ''world'' method of an SLxfig plot object:
<pre>
require("xfig");
variable p = xfig_plot_new();
p.world(x_grid[0], x_grid[-1], energy_grid[0]/1000, energy_grid[-1]/1000); % defining the coordinate system; energy in keV instead of eV
p.plot_png("banana.png");
p.xlabel("Sky X Position");
p.ylabel("Energy [keV]");
p.render("banana-plot.pdf");
</pre>
The resulting plot looks like this:

{{:isis:slxfig:banana-plot.png|banana-plot with coordinate system}}

Color-coded maps with 2d histograms, png, and xfig (xfig example)

2018-04-13T13:29:44Z

Sokolova-lapa:

[[Category:SLxfig]]
example added by Felix

There are many examples, where a color-coded map (or landscape) shows the results best, for example when showing the energy-dependence of the pulse profile of pulsar. All data depending on two parameters (in the example the count-rate depends on energy and on phase) can be displayed conveniently in this way. Another popular example is to show the χ² landscape as function of two fit-parameters on such a map instead of only showing the confidence contours.

A [[Example:_two-dimensional_histograms|second example]] illustrates [[Example:_two-dimensional_histograms|two-dimensional histograms]], which can be displayed in a very similar way.

=== Preparation ===
First of all, we need a 2d array A[y,x]. Let's stick to the energy dependent pulse profiles and assume we have four proiles pp1, pp2, pp3, and pp4 with 64 phase bins each, i.e pp# = Double_Type[64].
We could than produce A by writing
variable A = Double_Type[4,64] ;
A[0,*] = pp1 ; A[1,*] = pp2 ; A[2,*] = pp3 ; A[3,*] = pp4 ;

=== Making the image ===
The easiest way to plot a 2d array like that is to use
plot_image(A) ;
But this gives us only a black and white image of the array.

It's much nicer to use the S-lang "PNG" module, which allows to save the plot as a PNG file.
require("png") ; % not necessary if isisscripts have been loaded
First of all, we'd like to transfer our array to an image of RGB values. This can be achieved using a color map (the <code>png_get_colormap_names</code> function returns the names of all available color maps):
variable a_pic = png_gray_to_rgb(A, "rainbow") ;
Writing out is easy, just give the filename and the new array ''a_pic''
png_write_flipped("mymap.png", a_pic) ; % _flipped to get x and y axes right

=== Adding axes to the image ===
So far, so good, but the <code>mymap.png</code> is not really informative at the moment as it lacks the important information which parameters were plotted. This can be easily achieved by using the [[Plotting_with_the_S-Lang_Xfig_module|x-fig module]].

First we need to creat a new <code>xfig</code> structure:
require("xfig") ; % not necessary if isisscripts have been loaded
variable map = xfig_plot_new(11,11) ;

Define the coordinates <code>(xmin, xmax, ymin, ymax)</code>, assuming that pp1 starts at 5keV and pp4 ends at 100keV.
map.world(0, 1, 5, 100) ;

Load the PNG-file
map.plot_png("mymap.png") ;

Write labels
map.xlabel("Pulse phase") ;
map.ylabel("Energy [keV]") ;

Render all of that to an EPS file:
map.render("mymap.eps") ;

And voilá, <code>mymap.eps</code> contains our colorful map with the axes-labeled correctly.

=== Outlook ===
This example shows a very basic plot. It can quite easily extended, for example by plotting a scale next to it (for example [http://jedsoft.org/fun/slxfig/examples.html|SLxfig Plotting Examples, Example 6], click on the image to see the code). Or you could whish that the <code>y</code>-dimension of each pulse profile should represent its width in energy space, then you could make a new array with a lot of more rows in <code>y</code> direction, were you write in every row the same pulse profile between a given energy range. Or you could want to define your own colormap, this can be done with <code>png_add_colormap</code>.

The [[Example:_two-dimensional_histograms|second example]] illustrates [[Example:_two-dimensional_histograms|two-dimensional histograms]].

Two-dimensional histograms (xfig example)

2018-04-13T13:18:17Z

Sokolova-lapa:

[[Category:SLxfig]]

Plotting two-dimensional histograms using the png and xfig modules 
example added by Manfred

Similarly to the [[Example: color-coded maps with 2d histograms, png, and xfig|first example]] for creating [[Example: color-coded maps with 2d histograms, png, and xfig|color-coded maps]] with the [[Plotting_with_the_S-Lang_Xfig_module|SLxfig module]], the goal of this one is to produce a color-coded map,
but this time, the color-scale represents a density of (a possibly large number of) data points.

=== ISIS' histogram2d function ===

==== Usage ====
The <code>histogram2d</code> function is used in the following way (see also [http://pulsar.sternwarte.uni-erlangen.de/hanke/science/X-ray/ISIS/cgi/help.cgi?subj=histogram2d|help("histogram2d");]):
num = histogram2d(A, B, Agrid, Bgrid);
''A'' and ''B'' have to be ''Double_Type'' arrays of the same length,
''Agrid'' and ''Bgrid'' have to be ''Double_Type'' arrays with monotonically increasing elements.

Now, <code>num[a,b]</code> contains the number of points (<code>A</code>, <code>B</code>)
falling into each 2d-bin defined by the lower bin boundaries <code>Agrid[a]</code> and <code>Bgrid[b]</code>, i.e.:
num[a,b] == howmany( (Agrid[a] <= A < Agrid[a+1]) and (Bgrid[b] <= B < Bgrid[b+1]) );

==== Overflow bins ====
The last bin in each row or column is an //**overflow bin**// whose upper limit is at infinity, i.e.,
num[-1,b] == howmany( (Agrid[-1] <= A) and (Bgrid[b] <= B < Bgrid[b+1]) );
num[a,-1] == howmany( (Agrid[a] <= A < Agrid[a+1]) and (Bgrid[-1] <= B) );
and
num[-1,-1] == howmany( (Agrid[-1] <= A) and (Bgrid[-1] <= B) );

If one wants to remove these overflow bins,
one can simply apply the index-array ''[:-2]'' (which means "take all elements up to the second last one")
in both dimensions in order to create a smaller two-dimensional array:
num_ = num[ [:-2], [:-2] ];

The last bins corresponding to the reduced 2d-array ''num_'' //end// now at the same position where the grids //end//, too:
num_[-1,-1] == num[-2,-2] == howmany( (Agrid[-2] <= A < Agrid[-1]) and (Bgrid[-2] <= B < Bgrid[-1]) );
Before, the grids specified always lower bin boundaries,
but now, the grids have one element more than the correpsonding array-dimensions of ''num_''.

Note that ISIS (one-dimensional) ''histogram'' function does not produce an overflow bin.

==== Order of the indices ====
The first index of ''num'' (called ''a'' above) will always correspond
to the first [and third] argument of the ''histogram2d'' function (here called ''A'' [and ''Agrid'']),
and the second index (''b'') to the second [and fourth] argument (''B'' [and ''Bgrid'']).

As most functions that operate on two dimensional arrays (like ''plot_image'', ''png_write'', ''ds9_view'', ...)
expect that the //first index// of the 2d-array to correspond to the y-axis,
whereas only the //second index// to the x-axis,
one will have to pass the y-data [and -grid] before the x-data [and -grid]:
num = histogram2d(Y, X, Xgrid, Ygrid);

=== Using two-dimensional histograms ===

Just as in the [[isis:slxfig:ccmap|previous example]],
these two dimensional histograms can be transformed into a color-coded image,
which can then be included in an [[isis:slxfig|xfig plot]] which adds back the original coordinate system.

==== A "banana-plot" ====

In an X-ray gratings spectrometer (//Chandra//-HETGS, //XMM//-RGS),
the dispersion is not only proportional to the photon's wavelength, but also to the dispersion order.
Different orders, however, can be separated with the internal energy resolution of the CCD detector.

The following example plots the density of events in a position--energy diagram:

===== Writing the png image =====

<pre>
variable evts = fits_read_table("evt2.fits"); % reading a Chandra level-2 event file

variable x_grid = [2300:5700:#320]; % x position on the detector (320 values)
variable energy_grid = [0:10000:#240]; % energies in eV (240 values from 0 to 10 keV)

variable num = histogram2d(evts.energy, evts.x, % the data (Y, X)
energy_grid, x_grid % the grids (Ygrid, Xgrid)
)[[:-2],[:-2]]; % removing overflow bins

require("png"); % load png module
variable RGB = png_gray_to_rgb(log(1+num), "ds9sls"); % transform num values logarithmically to RGB values, using the ds9sls color map
png_write_flipped("banana.png", RGB); % write RGB values to a png file
% png_write_flipped places RGB[0,0] in the *lower* left corner
</pre>
This produces just the bare image "banana.png":

{{:isis:slxfig:banana.png|bare image "banana.png"}}

With the [[isis:slxfig|S-Lang xfig module]], the coordinate system can, however, be easily added (back again).

===== Plotting the png into an SLxfig plot =====

It is important to set the correct coordinates for the SLxfig plot object,
as this information is no more present in the bare image.
As discussed above (in the section on "overflow bins"),
the last bins of the reduced 2d-array end where the original grids end
-- and obviously the first bins start where the grids start.
This is all the information that needs to be passed to the ''world'' method of an SLxfig plot object:
<pre>
require("xfig");
variable p = xfig_plot_new();
p.world(x_grid[0], x_grid[-1], energy_grid[0]/1000, energy_grid[-1]/1000); % defining the coordinate system; energy in keV instead of eV
p.plot_png("banana.png");
p.xlabel("Sky X Position");
p.ylabel("Energy [keV]");
p.render("banana-plot.pdf");
</pre>
The resulting plot looks like this:

{{:isis:slxfig:banana-plot.png|banana-plot with coordinate system}}

Color-coded maps with 2d histograms, png, and xfig (xfig example)

2018-04-13T13:04:04Z

Sokolova-lapa:

[[Category:SLxfig]]
example added by Felix

There are many examples, where a color-coded map (or landscape) shows the results best, for example when showing the energy-dependence of the pulse profile of pulsar. All data depending on two parameters (in the example the count-rate depends on energy and on phase) can be displayed conveniently in this way. Another popular example is to show the χ² landscape as function of two fit-parameters on such a map instead of only showing the confidence contours.

A [[Example:_two-dimensional_histograms|second example]] illustrates [[Example:_two-dimensional_histograms|two-dimensional histograms]], which can be displayed in a very similar way.

=== Preparation ===
First of all, we need a 2d array A[y,x]. Let's stick to the energy dependent pulse profiles and assume we have four proiles pp1, pp2, pp3, and pp4 with 64 phase bins each, i.e pp# = Double_Type[64].
We could than produce A by writing
variable A = Double_Type[4,64] ;
A[0,*] = pp1 ; A[1,*] = pp2 ; A[2,*] = pp3 ; A[3,*] = pp4 ;

=== Making the image ===
The easiest way to plot a 2d array like that is to use
plot_image(A) ;
But this gives us only a black and white image of the array.

It's much nicer to use the S-lang "PNG" module, which allows to save the plot as a PNG file.
require("png") ; % not necessary if isisscripts have been loaded
First of all, we'd like to transfer our array to an image of RGB values. This can be achieved using a color map (the <code>png_get_colormap_names</code> function returns the names of all available color maps):
variable a_pic = png_gray_to_rgb(A, "rainbow") ;
Writing out is easy, just give the filename and the new array ''a_pic''
png_write_flipped("mymap.png", a_pic) ; % _flipped to get x and y axes right

=== Adding axes to the image ===
So far, so good, but the <code>mymap.png</code> is not really informative at the moment as it lacks the important information which parameters were plotted. This can be easily achieved by using the [[Plotting_with_the_S-Lang_Xfig_module|x-fig module]].

First we need to creat a new <code>xfig</code> structure:
require("xfig") ; % not necessary if isisscripts have been loaded
variable map = xfig_plot_new(11,11) ;

Define the coordinates <code>(xmin, xmax, ymin, ymax)</code>, assuming that pp1 starts at 5keV and pp4 ends at 100keV.
map.world(0, 1, 5, 100) ;

Load the PNG-file
map.plot_png("mymap.png") ;

Write labels
map.xlabel("Pulse phase") ;
map.ylabel("Energy [keV]") ;

Render all of that to an EPS file:
map.render("mymap.eps") ;

And voilá, <code>mymap.eps</code> contains our colorful map with the axes-labeled correctly.

=== Outlook ===
This example shows a very basic plot. It can quite easily extended, for example by plotting a scale next to it (for example [http://jedsoft.org/fun/slxfig/examples.html|SLxfig Plotting Examples, Example 6], click on the image to see the code). Or you could whish that the <code>y</code>-dimension of each pulse profile should represent its width in energy space, then you could make a new array with a lot of more rows in <code>y</code> direction, were you write in every row the same pulse profile between a given energy range. Or you could want to define your own colormap, this can be done with <code>png_add_colormap</code>.

The [[Example:_two-dimensional_histograms|second example]] illustrates [[Example:_two-dimensional_histograms|two-dimensional histograms]].

Plotting with the S-Lang Xfig module

2018-04-13T13:03:42Z

Sokolova-lapa:

SLxfig will not usually come with your standard ISIS installation, but it's an easy to install module. Get it from [http://www.jedsoft.org/fun/slxfig/ JedSoft/Xfig]

=== Overview of subtopics (examples) ===
* [[Example: color-coded maps with 2d histograms, png, and xfig]]
* [[Example:_two-dimensional_histograms|Example: two-dimensional histograms]]
* [[isis:slxfig:multiplot|Example: compounds and multi-panel plots]]
* [[isis:slxfig:insetplot|Example: plot within in a plot (inset)]]
* [[isis:slxfig:fancy_plots|Example: plotting spectra in the way of Mike's fancy plots]]
* [[isis:slxfig:plot_components|Example: plotting individual components of a model]]

And most important
* [[Isis_slxfig_fancyremeisplots| The Remeis X-fig plot gallery ]]

Note also the examples on the SLxfig websites of [http://www.jedsoft.org/fun/slxfig/examples.html John E. Davis]
and [http://pulsar.sternwarte.uni-erlangen.de/hanke/science/X-ray/ISIS/SLxfig/ Manfred Hanke].

--- ''Manfred's notes from his first introduction on 2010-04-28'' --- (to be continued?)

== General Tips & Tricks ==

If you never plotted with slxfig, please have a look at the next section.

=== Random pieces of helpful code: ===

* Prevent the ticlabels from exceeding the plot size: <tt>pl.axis(;ticlabels_confine);</tt>
* Format ticlabels:
** linear scale: to e.g. 2 places after decimal point: ''pl.axis(;linear, format="$%.2f$");''
** log scale: to e.g. 2 places after decimal point in power of number: ''pl.axis(; log, format="$10^{%+.2f}$");'' where the ''+'' tells to always show the sign of the power

=== eps-Files with slxfig ===
(''after Jörns Mail'')

The eps produced by the slxfig module is usually '''VERY large''' because the postscript
code produced by transfig is very inefficient. With some postprocessing
you can significantly reduce the figure sizes:

- convert your figure to pdf (the -dEPSCrop is important - this tells ps2pdf to use the eps bounding box): <code>ps2pdf -dEPSCrop bla.eps</code>

- if you really need postscript, e.g., for a journal submission where pdf figures are not allowed, then convert the pdf back to (encapsulated) postscript: <code>pdf2ps -dLanguageLevel=3 bla.pdf bla.ps</code>

a few numbers:

* original eps file size: 3.9MB
* pdf file size: 37kB
* eps file size after converting back: 187kB

=== the autoeps and tmp folders ===

The autoeps and tmp folders are always created by default in the folder you're executing your script. These folders contain caching information such that plotting of the same or similar things doesn't have to be done over and over again from scratch. As you have them in each folder separately, these folders tend to be annoying. Either you're deleting the folders occasionally, or you spent quite some amount of disk space for really useless stuff. The solution is to tell slxfig to create these folders in a specifc location. There they don't take up space on /home or /userdata and don't appear in your scripting folders.

So, in order to achieve this you have to do the following:

# Create a file named ".slxfigrc" in your home directory
# Add the lines
<pre>
variable slxfig_tmp_dir;
if (stat_file("/scratch1") == NULL) {
slxfig_tmp_dir = "/tmp/"+getenv("USER")+"/xfig/";
} else {
slxfig_tmp_dir = "/scratch1/"+getenv("USER")+"/xfig/";
}
xfig_set_tmp_dir(slxfig_tmp_dir);
xfig_set_autoeps_dir(slxfig_tmp_dir);
</pre>

Then all the temporary files in all of your slxfig scripts will from now
on be stored in these directories.

Note that this more complicated setup is done in order to avoid putting files on /tmp, if a /scratch1 file system exists. The reason being that too many files on /tmp might crash your computer, as there is a maximal number of files that can be on a certain disk. And /tmp is located on the disk where the operating system is installed. And now just imagine the chaos when the system itself is not able to write any more files ... so better use a different disk (that means the /scratch1 disk) for the SLxfig tmp files, by following the approach above.

=== Programming preliminaries ===

==== References in S-Lang ====

===== References to variables =====

Functions cannot change scalar arguments that are passed by value:
<pre>
define test(v)
{ vmessage("in test: v=%d", v);
v = -1; % only modifies variable local to test
vmessage("in test: v=%d", v);
}

variable a=42;
test(a); % a is passed by value
vmessage("a=%d", a); % a has not been changed outside of test
test(42); % test can also be run with a constant
</pre>
reference operator ''&'', dereference operator ''@'':
<pre>
variable r = &a; % reference to a (from previous example)
vmessage("r=%S; @r=%d", r, @r); % reference and dereferenced reference
</pre>
references to variables:
<pre>
define test2(r)
{ vmessage("in test: @r=%d", @r);
% r is still only a local variable
@r = -1; % r is not changed, but the variable referenced by r
vmessage("in test: @r=%d", @r);
}

test2(&a); % (from previous examples)
vmessage("a=%d", a); % a *has* been changed
</pre>

[[isis:references|see also]]

===== References to functions =====
<pre>
variable my_fun = &sin;
print( @my_fun(0) );
print( @my_fun(PI/2) );

variable x=[0:10:0.01];
plot(x, @my_fun(x));

my_fun = &exp;
plot(x, @my_fun(x));
</pre>

==== Object-oriented programming ====

The following function only operates on "car-structures":
<pre>
define drive_car(c, dest)
{
vmessage("%s drives from %s to %s", c.plate, c.place, dest);
c.place = dest;
}

define init_car(plate, place)
{
return struct { plate=plate, place=place };
}

variable car = init_car("S-FR 3011", "Erlangen");
drive_car(car, "Bamberg");
drive_car(car, "Erlangen");
</pre>

It should thus be more directly connected to such an object.
=> Define a new field of the structure with reference to the function:

<pre>
define init_car(plate, place)
{
return struct { plate=plate, place=place, drive=&drive_car };
}

variable car = init_car("S-FR 3011", "Erlangen");
(@car.drive)(car, "Bamberg"); % @car.drive is actually the function drive_car
</pre>

=== OO in S-Lang ===

from the S-Lang manual, Appendix A.3 ''What's new for S-Lang 2.0:''

Syntactic sugar for objected-oriented style method calls.
S-Lang 1 code such as
<code>(@s.method)(s, args);</code>
may be written much more simply as
<code>s.method(args);</code>
This should make "object-oriented" code somewhat more readable.

<code>car.drive("Erlangen"); % car is implicitly passed as first argument to drive_car</code>

=== Xfig ===

http://www.xfig.org/

===== The S-Lang xfig module =====

see [http://jedsoft.org/fun/slxfig/ John E. Davis' homepage],
especially the [http://jedsoft.org/fun/slxfig/examples.html examples page]

The examples from the git repository
git://git.jedsoft.org/git/slxfig.git
(or my ''Mh'' branch on [http://www.sternwarte.uni-erlangen.de/~hanke/git.public/?p=slxfig;a=shortlog;h=Mh http://www.sternwarte.uni-erlangen.de/~hanke/git.public/slxfig])
are also available on http://pulsar.sternwarte.uni-erlangen.de/hanke/science/X-ray/ISIS/SLxfig/.

==== Xfig objects as OO-style S-Lang structures ====
<pre>
variable po = xfig_new_polygon([0, 2, 1, 0], [0, 0, 2, 0]);
print(po); % structure with many internal fields
% and methods (function references) that should be used as interface
po.render("polygon.eps"); % writes .fig file, runs xfig to produce output

po.set_fill_color("red");
po.set_area_fill(20);
po.render("polygon_red.eps");
</pre>
{{:isis:slxfig:polygon.eps|polygon}}
{{:isis:slxfig:polygon_red.eps|polygon_red}}

==== High-level plot objects ====
<pre>
variable pl = xfig_plot_new();
variable x = [0:10:0.01];
pl.plot(x, sin(x)); % x-y plot
pl.title("a nice sine wave $y=\sin(x)$"R); % SLxfig renders text via latex
pl.xlabel("$x$");
pl.ylabel("$y$");
pl.render("plot.pdf"); % run XFig's fig2dev to create an pdf file
pl.render("plot.eps"); % run XFig's fig2dev to create an eps file
pl.render("plot.png"); % run XFig's fig2dev to create a png
</pre>
[[File:plot.png|plot]]

define world coordinate system(s):
<pre>
variable pl2 = xfig_plot_new(7, 5); % size of the plot window in cm x cm (default is 14 cm x 10 cm)
pl2.world(-2, 12, -1.5, 1.5);
pl2.world2(-2/PI, 12/PI, -1.5, 1.5);
pl2.plot(x, sin(x));
pl2.render("plot2.eps");
</pre>
{{:isis:slxfig:plot2.eps|plot2}}

configuration of the axes via qualifiers
<pre>
variable pl3 = xfig_plot_new(7, 5);
pl3.world(-2, 12, -1.5, 1.5);
pl3.world2(-2/PI, 12/PI, -1.5, 1.5);
pl3.y2axis(; off); % totally switch off y2-axis
pl3.y1axis(; ticlabels=0); % only remove y1 tic mark labels
pl3.x2axis(; major=[0, PI/2, PI]); % define own major tic marks
pl3.x1axis(; major=[-1, 5, 11], minor=[-5:15:0.5]); % But then, one (currently) also has to define the minor tic marks!
pl3.plot(x, sin(x));
pl3.render("plot3.eps");
</pre>
{{:isis:slxfig:plot3.eps|plot3}}

I'm trying to document these functions.
Suggested syntax for methods of objects:
<code>help("xfig_plot.x1axis");</code>
Or directly from the method itself:
<code>pl.x1axis(; help);</code>

[[Category:SLxfig]]
[[Category:Isis / Slang]]

Color-coded maps with 2d histograms, png, and xfig (xfig example)

2018-04-13T12:57:43Z

Sokolova-lapa:

[[Category:SLxfig]]
example added by Felix

There are many examples, where a color-coded map (or landscape) shows the results best, for example when showing the energy-dependence of the pulse profile of pulsar. All data depending on two parameters (in the example the count-rate depends on energy and on phase) can be displayed conveniently in this way. Another popular example is to show the χ² landscape as function of two fit-parameters on such a map instead of only showing the confidence contours.

A [[Example:_two-dimensional_histograms|second example]] illustrates [[Example:_two-dimensional_histograms|two-dimensional histograms]], which can be displayed in a very similar way.

=== Preparation ===
First of all, we need a 2d array A[y,x]. Let's stick to the energy dependent pulse profiles and assume we have four proiles pp1, pp2, pp3, and pp4 with 64 phase bins each, i.e pp# = Double_Type[64].
We could than produce A by writing
variable A = Double_Type[4,64] ;
A[0,*] = pp1 ; A[1,*] = pp2 ; A[2,*] = pp3 ; A[3,*] = pp4 ;

=== Making the image ===
The easiest way to plot a 2d array like that is to use
plot_image(A) ;
But this gives us only a black and white image of the array.

It's much nicer to use the S-lang "PNG" module, which allows to save the plot as a PNG file.
require("png") ; % not necessary if isisscripts have been loaded
First of all, we'd like to transfer our array to an image of RGB values. This can be achieved using a color map (the <code>png_get_colormap_names</code> function returns the names of all available color maps):
variable a_pic = png_gray_to_rgb(A, "rainbow") ;
Writing out is easy, just give the filename and the new array ''a_pic''
png_write_flipped("mymap.png", a_pic) ; % _flipped to get x and y axes right

=== Adding axes to the image ===
So far, so good, but the <code>mymap.png</code> is not really informative at the moment as it lacks the important information which parameters were plotted. This can be easily achieved by using the [[Plotting_with_the_S-Lang_Xfig_module|x-fig module]].

First we need to creat a new <code>xfig</code> structure:
require("xfig") ; % not necessary if isisscripts have been loaded
variable map = xfig_plot_new(11,11) ;

Define the coordinates <code>(xmin, xmax, ymin, ymax)</code>, assuming that pp1 starts at 5keV and pp4 ends at 100keV.
map.world(0, 1, 5, 100) ;

Load the PNG-file
map.plot_png("mymap.png") ;

Write labels
map.xlabel("Pulse phase") ;
map.ylabel("Energy [keV]") ;

Render all of that to an EPS file:
map.render("mymap.eps") ;

And voilá, <code>mymap.eps</code> contains our colorful map with the axes-labeled correctly.

=== Outlook ===
This example shows a very basic plot. It can quite easily extended, for example by plotting a scale next to it (for example [[http://jedsoft.org/fun/slxfig/examples.html|SLxfig Plotting Examples, Example 6]], click on the image to see the code). Or you could whish that the <code>y</code>-dimension of each pulse profile should represent its width in energy space, then you could make a new array with a lot of more rows in <code>y</code> direction, were you write in every row the same pulse profile between a given energy range. Or you could want to define your own colormap, this can be done with <code>png_add_colormap</code>.

The [[Example:_two-dimensional_histograms|second example]] illustrates [[Example:_two-dimensional_histograms|two-dimensional histograms]].

Color-coded maps with 2d histograms, png, and xfig (xfig example)

2018-04-13T12:54:15Z

Sokolova-lapa:

[[Category:SLxfig]]
-- example added by Felix --

There are many examples, where a color-coded map (or landscape) shows the results best, for example when showing the energy-dependence of the pulse profile of pulsar. All data depending on two parameters (in the example the count-rate depends on energy and on phase) can be displayed conveniently in this way. Another popular example is to show the χ² landscape as function of two fit-parameters on such a map instead of only showing the confidence contours.

A [[Example:_two-dimensional_histograms|second example]] illustrates [[Example:_two-dimensional_histograms|two-dimensional histograms]], which can be displayed in a very similar way.

=== Preparation ===
First of all, we need a 2d array A[y,x]. Let's stick to the energy dependent pulse profiles and assume we have four proiles pp1, pp2, pp3, and pp4 with 64 phase bins each, i.e pp# = Double_Type[64].
We could than produce A by writing
variable A = Double_Type[4,64] ;
A[0,*] = pp1 ; A[1,*] = pp2 ; A[2,*] = pp3 ; A[3,*] = pp4 ;

=== Making the image ===
The easiest way to plot a 2d array like that is to use
plot_image(A) ;
But this gives us only a black and white image of the array.

It's much nicer to use the S-lang "PNG" module, which allows to save the plot as a PNG file.
require("png") ; % not necessary if isisscripts have been loaded
First of all, we'd like to transfer our array to an image of RGB values. This can be achieved using a color map (the <code>png_get_colormap_names</code> function returns the names of all available color maps):
variable a_pic = png_gray_to_rgb(A, "rainbow") ;
Writing out is easy, just give the filename and the new array ''a_pic''
png_write_flipped("mymap.png", a_pic) ; % _flipped to get x and y axes right

=== Adding axes to the image ===
So far, so good, but the <code>mymap.png</code> is not really informative at the moment as it lacks the important information which parameters were plotted. This can be easily achieved by using the [[Plotting_with_the_S-Lang_Xfig_module|x-fig module]].

First we need to creat a new <code>xfig</code> structure:
require("xfig") ; % not necessary if isisscripts have been loaded
variable map = xfig_plot_new(11,11) ;

Define the coordinates <code>(xmin, xmax, ymin, ymax)</code>, assuming that pp1 starts at 5keV and pp4 ends at 100keV.
map.world(0, 1, 5, 100) ;

Load the PNG-file
map.plot_png("mymap.png") ;

Write labels
map.xlabel("Pulse phase") ;
map.ylabel("Energy [keV]") ;

Render all of that to an EPS file:
map.render("mymap.eps") ;

And voilá, <code>mymap.eps</code> contains our colorful map with the axes-labeled correctly.

===== Outlook =====
This example shows a very basic plot. It can quite easily extended, for example by plotting a scale next to it (for example [[http://jedsoft.org/fun/slxfig/examples.html|SLxfig Plotting Examples, Example 6]], click on the image to see the code). Or you could whish that the <code>y</code>-dimension of each pulse profile should represent its width in energy space, then you could make a new array with a lot of more rows in <code>y</code> direction, were you write in every row the same pulse profile between a given energy range. Or you could want to define your own colormap, this can be done with <code>png_add_colormap</code>.

The [[Example:_two-dimensional_histograms|second example]] illustrates [[Example:_two-dimensional_histograms|two-dimensional histograms]].

Two-dimensional histograms (xfig example)

2018-04-13T10:34:55Z

Sokolova-lapa: Created page with " Category:SLxfig === Plotting two-dimensional histograms using the png and xfig modules === --- //example added by Manfred// --- Similarly to the isis:slxfig:ccmap|..."

[[Category:SLxfig]]

=== Plotting two-dimensional histograms using the png and xfig modules ===

--- //example added by Manfred// ---

Similarly to the [[isis:slxfig:ccmap|first example]] for creating [[isis:slxfig:ccmap|color-coded maps]] with the [[isis:slxfig|SLxfig module]], the goal of this one is to produce a color-coded map,
but this time, the color-scale represents a density of (a possibly large number of) data points.

=== ISIS' histogram2d function ===

==== Usage ====
The ''histogram2d'' function is used in the following way (see also [[http://pulsar.sternwarte.uni-erlangen.de/hanke/science/X-ray/ISIS/cgi/help.cgi?subj=histogram2d|help("histogram2d");]]):
num = histogram2d(A, B, Agrid, Bgrid);
''A'' and ''B'' have to be ''Double_Type'' arrays of the same length,
''Agrid'' and ''Bgrid'' have to be ''Double_Type'' arrays with monotonically increasing elements.

Now, ''num[a,b]'' contains the **number of points** (''A'', ''B'')
falling into each 2d-bin defined by the lower bin boundaries ''Agrid[a]'' and ''Bgrid[b]'', i.e.:
num[a,b] == howmany( (Agrid[a] <= A < Agrid[a+1]) and (Bgrid[b] <= B < Bgrid[b+1]) );

==== Overflow bins ====
The last bin in each row or column is an //**overflow bin**// whose upper limit is at infinity, i.e.,
num[-1,b] == howmany( (Agrid[-1] <= A) and (Bgrid[b] <= B < Bgrid[b+1]) );
num[a,-1] == howmany( (Agrid[a] <= A < Agrid[a+1]) and (Bgrid[-1] <= B) );
and
num[-1,-1] == howmany( (Agrid[-1] <= A) and (Bgrid[-1] <= B) );

If one wants to remove these overflow bins,
one can simply apply the index-array ''[:-2]'' (which means "take all elements up to the second last one")
in both dimensions in order to create a smaller two-dimensional array:
num_ = num[ [:-2], [:-2] ];

The last bins corresponding to the reduced 2d-array ''num_'' //end// now at the same position where the grids //end//, too:
num_[-1,-1] == num[-2,-2] == howmany( (Agrid[-2] <= A < Agrid[-1]) and (Bgrid[-2] <= B < Bgrid[-1]) );
Before, the grids specified always lower bin boundaries,
but now, the grids have one element more than the correpsonding array-dimensions of ''num_''.

Note that ISIS (one-dimensional) ''histogram'' function does not produce an overflow bin.

==== Order of the indices ====
The first index of ''num'' (called ''a'' above) will always correspond
to the first [and third] argument of the ''histogram2d'' function (here called ''A'' [and ''Agrid'']),
and the second index (''b'') to the second [and fourth] argument (''B'' [and ''Bgrid'']).

As most functions that operate on two dimensional arrays (like ''plot_image'', ''png_write'', ''ds9_view'', ...)
expect that the //first index// of the 2d-array to correspond to the y-axis,
whereas only the //second index// to the x-axis,
one will have to pass the y-data [and -grid] before the x-data [and -grid]:
num = histogram2d(Y, X, Xgrid, Ygrid);

=== Using two-dimensional histograms ===

Just as in the [[isis:slxfig:ccmap|previous example]],
these two dimensional histograms can be transformed into a color-coded image,
which can then be included in an [[isis:slxfig|xfig plot]] which adds back the original coordinate system.

==== A "banana-plot" ====

In an X-ray gratings spectrometer (//Chandra//-HETGS, //XMM//-RGS),
the dispersion is not only proportional to the photon's wavelength, but also to the dispersion order.
Different orders, however, can be separated with the internal energy resolution of the CCD detector.

The following example plots the density of events in a position--energy diagram:

===== Writing the png image =====

<pre>
variable evts = fits_read_table("evt2.fits"); % reading a Chandra level-2 event file

variable x_grid = [2300:5700:#320]; % x position on the detector (320 values)
variable energy_grid = [0:10000:#240]; % energies in eV (240 values from 0 to 10 keV)

variable num = histogram2d(evts.energy, evts.x, % the data (Y, X)
energy_grid, x_grid % the grids (Ygrid, Xgrid)
)[[:-2],[:-2]]; % removing overflow bins

require("png"); % load png module
variable RGB = png_gray_to_rgb(log(1+num), "ds9sls"); % transform num values logarithmically to RGB values, using the ds9sls color map
png_write_flipped("banana.png", RGB); % write RGB values to a png file
% png_write_flipped places RGB[0,0] in the *lower* left corner
</pre>
This produces just the bare image "banana.png":

{{:isis:slxfig:banana.png|bare image "banana.png"}}

With the [[isis:slxfig|S-Lang xfig module]], the coordinate system can, however, be easily added (back again).

===== Plotting the png into an SLxfig plot =====

It is important to set the correct coordinates for the SLxfig plot object,
as this information is no more present in the bare image.
As discussed above (in the section on "overflow bins"),
the last bins of the reduced 2d-array end where the original grids end
-- and obviously the first bins start where the grids start.
This is all the information that needs to be passed to the ''world'' method of an SLxfig plot object:
<pre>
require("xfig");
variable p = xfig_plot_new();
p.world(x_grid[0], x_grid[-1], energy_grid[0]/1000, energy_grid[-1]/1000); % defining the coordinate system; energy in keV instead of eV
p.plot_png("banana.png");
p.xlabel("Sky X Position");
p.ylabel("Energy [keV]");
p.render("banana-plot.pdf");
</pre>
The resulting plot looks like this:

{{:isis:slxfig:banana-plot.png|banana-plot with coordinate system}}

Color-coded maps with 2d histograms, png, and xfig (xfig example)

2018-04-13T10:29:47Z

Sokolova-lapa:

[[Category:SLxfig]]
-- example added by Felix --

There are many examples, where a color-coded map (or landscape) shows the results best, for example when showing the energy-dependence of the pulse profile of pulsar. All data depending on two parameters (in the example the count-rate depends on energy and on phase) can be displayed conveniently in this way. Another popular example is to show the χ² landscape as function of two fit-parameters on such a map instead of only showing the confidence contours.

A [[isis:slxfig:histogram2d|second example]] illustrates [[isis:slxfig:histogram2d|two-dimensional histograms]], which can be displayed in a very similar way.

=== Preparation ===
First of all, we need a 2d array A[y,x]. Let's stick to the energy dependent pulse profiles and assume we have four proiles pp1, pp2, pp3, and pp4 with 64 phase bins each, i.e pp# = Double_Type[64].
We could than produce A by writing
variable A = Double_Type[4,64] ;
A[0,*] = pp1 ; A[1,*] = pp2 ; A[2,*] = pp3 ; A[3,*] = pp4 ;

=== Making the image ===
The easiest way to plot a 2d array like that is to use
plot_image(A) ;
But this gives us only a black and white image of the array.

It's much nicer to use the S-lang "PNG" module, which allows to save the plot as a PNG file.
require("png") ; % not necessary if isisscripts have been loaded
First of all, we'd like to transfer our array to an image of RGB values. This can be achieved using a color map (the ''png_get_colormap_names'' function returns the names of all available color maps):
variable a_pic = png_gray_to_rgb(A, "rainbow") ;
Writing out is easy, just give the filename and the new array ''a_pic''
png_write_flipped("mymap.png", a_pic) ; % _flipped to get x and y axes right

=== Adding axes to the image ===
So far, so good, but the ''mymap.png'' is not really informative at the moment as it lacks the important information which parameters were plotted. This can be easily achieved by using the [[isis:slxfig|x-fig module]].

First we need to creat a new ''xfig'' structure:
require("xfig") ; % not necessary if isisscripts have been loaded
variable map = xfig_plot_new(11,11) ;

Define the coordinates ''(xmin, xmax, ymin, ymax)'', assuming that pp1 starts at 5keV and pp4 ends at 100keV.
map.world(0, 1, 5, 100) ;

Load the PNG-file
map.plot_png("mymap.png") ;

Write labels
map.xlabel("Pulse phase") ;
map.ylabel("Energy [keV]") ;

Render all of that to an EPS file:
map.render("mymap.eps") ;

And voilá, ''mymap.eps'' contains our colorful map with the axes-labeled correctly.

===== Outlook =====
This example shows a very basic plot. It can quite easily extended, for example by plotting a scale next to it (for example [[http://jedsoft.org/fun/slxfig/examples.html|SLxfig Plotting Examples, Example 6]], click on the image to see the code). Or you could whish that the ''y''-dimension of each pulse profile should represent its width in energy space, then you could make a new array with a lot of more rows in ''y'' direction, were you write in every row the same pulse profile between a given energy range. Or you could want to define your own colormap, this can be done with ''png_add_colormap''.

The [[isis:slxfig:histogram2d|second example]] illustrates [[isis:slxfig:histogram2d|two-dimensional histograms]].

Color-coded maps with 2d histograms, png, and xfig (xfig example)

2018-04-13T10:29:30Z

Sokolova-lapa:

[[Category:SLxfig]]

-- example added by Felix --

There are many examples, where a color-coded map (or landscape) shows the results best, for example when showing the energy-dependence of the pulse profile of pulsar. All data depending on two parameters (in the example the count-rate depends on energy and on phase) can be displayed conveniently in this way. Another popular example is to show the χ² landscape as function of two fit-parameters on such a map instead of only showing the confidence contours.

A [[isis:slxfig:histogram2d|second example]] illustrates [[isis:slxfig:histogram2d|two-dimensional histograms]], which can be displayed in a very similar way.

=== Preparation ===
First of all, we need a 2d array A[y,x]. Let's stick to the energy dependent pulse profiles and assume we have four proiles pp1, pp2, pp3, and pp4 with 64 phase bins each, i.e pp# = Double_Type[64].
We could than produce A by writing
variable A = Double_Type[4,64] ;
A[0,*] = pp1 ; A[1,*] = pp2 ; A[2,*] = pp3 ; A[3,*] = pp4 ;

=== Making the image ===
The easiest way to plot a 2d array like that is to use
plot_image(A) ;
But this gives us only a black and white image of the array.

It's much nicer to use the S-lang "PNG" module, which allows to save the plot as a PNG file.
require("png") ; % not necessary if isisscripts have been loaded
First of all, we'd like to transfer our array to an image of RGB values. This can be achieved using a color map (the ''png_get_colormap_names'' function returns the names of all available color maps):
variable a_pic = png_gray_to_rgb(A, "rainbow") ;
Writing out is easy, just give the filename and the new array ''a_pic''
png_write_flipped("mymap.png", a_pic) ; % _flipped to get x and y axes right

=== Adding axes to the image ===
So far, so good, but the ''mymap.png'' is not really informative at the moment as it lacks the important information which parameters were plotted. This can be easily achieved by using the [[isis:slxfig|x-fig module]].

First we need to creat a new ''xfig'' structure:
require("xfig") ; % not necessary if isisscripts have been loaded
variable map = xfig_plot_new(11,11) ;

Define the coordinates ''(xmin, xmax, ymin, ymax)'', assuming that pp1 starts at 5keV and pp4 ends at 100keV.
map.world(0, 1, 5, 100) ;

Load the PNG-file
map.plot_png("mymap.png") ;

Write labels
map.xlabel("Pulse phase") ;
map.ylabel("Energy [keV]") ;

Render all of that to an EPS file:
map.render("mymap.eps") ;

And voilá, ''mymap.eps'' contains our colorful map with the axes-labeled correctly.

===== Outlook =====
This example shows a very basic plot. It can quite easily extended, for example by plotting a scale next to it (for example [[http://jedsoft.org/fun/slxfig/examples.html|SLxfig Plotting Examples, Example 6]], click on the image to see the code). Or you could whish that the ''y''-dimension of each pulse profile should represent its width in energy space, then you could make a new array with a lot of more rows in ''y'' direction, were you write in every row the same pulse profile between a given energy range. Or you could want to define your own colormap, this can be done with ''png_add_colormap''.

The [[isis:slxfig:histogram2d|second example]] illustrates [[isis:slxfig:histogram2d|two-dimensional histograms]].

Color-coded maps with 2d histograms, png, and xfig (xfig example)

2018-04-13T10:27:25Z

Sokolova-lapa: Created page with " Category:SLxfig = Example: plotting color-coded maps with the png and xfig modules = -- example added by Felix -- There are many examples, where a color-coded map (or..."

[[Category:SLxfig]]

= Example: plotting color-coded maps with the png and xfig modules =
-- example added by Felix --

There are many examples, where a color-coded map (or landscape) shows the results best, for example when showing the energy-dependence of the pulse profile of pulsar. All data depending on two parameters (in the example the count-rate depends on energy and on phase) can be displayed conveniently in this way. Another popular example is to show the χ² landscape as function of two fit-parameters on such a map instead of only showing the confidence contours.

A [[isis:slxfig:histogram2d|second example]] illustrates [[isis:slxfig:histogram2d|two-dimensional histograms]], which can be displayed in a very similar way.

=== Preparation ===
First of all, we need a 2d array A[y,x]. Let's stick to the energy dependent pulse profiles and assume we have four proiles pp1, pp2, pp3, and pp4 with 64 phase bins each, i.e pp# = Double_Type[64].
We could than produce A by writing
variable A = Double_Type[4,64] ;
A[0,*] = pp1 ; A[1,*] = pp2 ; A[2,*] = pp3 ; A[3,*] = pp4 ;

=== Making the image ===
The easiest way to plot a 2d array like that is to use
plot_image(A) ;
But this gives us only a black and white image of the array.

It's much nicer to use the S-lang "PNG" module, which allows to save the plot as a PNG file.
require("png") ; % not necessary if isisscripts have been loaded
First of all, we'd like to transfer our array to an image of RGB values. This can be achieved using a color map (the ''png_get_colormap_names'' function returns the names of all available color maps):
variable a_pic = png_gray_to_rgb(A, "rainbow") ;
Writing out is easy, just give the filename and the new array ''a_pic''
png_write_flipped("mymap.png", a_pic) ; % _flipped to get x and y axes right

=== Adding axes to the image ===
So far, so good, but the ''mymap.png'' is not really informative at the moment as it lacks the important information which parameters were plotted. This can be easily achieved by using the [[isis:slxfig|x-fig module]].

First we need to creat a new ''xfig'' structure:
require("xfig") ; % not necessary if isisscripts have been loaded
variable map = xfig_plot_new(11,11) ;

Define the coordinates ''(xmin, xmax, ymin, ymax)'', assuming that pp1 starts at 5keV and pp4 ends at 100keV.
map.world(0, 1, 5, 100) ;

Load the PNG-file
map.plot_png("mymap.png") ;

Write labels
map.xlabel("Pulse phase") ;
map.ylabel("Energy [keV]") ;

Render all of that to an EPS file:
map.render("mymap.eps") ;

And voilá, ''mymap.eps'' contains our colorful map with the axes-labeled correctly.

===== Outlook =====
This example shows a very basic plot. It can quite easily extended, for example by plotting a scale next to it (for example [[http://jedsoft.org/fun/slxfig/examples.html|SLxfig Plotting Examples, Example 6]], click on the image to see the code). Or you could whish that the ''y''-dimension of each pulse profile should represent its width in energy space, then you could make a new array with a lot of more rows in ''y'' direction, were you write in every row the same pulse profile between a given energy range. Or you could want to define your own colormap, this can be done with ''png_add_colormap''.

The [[isis:slxfig:histogram2d|second example]] illustrates [[isis:slxfig:histogram2d|two-dimensional histograms]].

XPRA and SSH

2018-04-11T14:27:49Z

Sokolova-lapa:

[[Category:Working Remotely]]

= Working remotely using XPRA and SSH =

[https://www.xpra.org/ XPRA] allows you to start remote X programs and display them on your local machine. [[Winswitch|Winswitch]] uses XPRA internally, but you can use it directly as well. Especially, you can use the speed of [[SSH|SSH]] for commands, but don't need to use X11-forwarding during your SSH-connection, which can be very slow.

First, you need to install XPRA on your local machine. If you are using a Debian-based UNIX-system you can get XPRA via
<pre>
sudo apt-get install xpra
</pre>
Please note that you might not get the current version of XPRA depending on your distribution. Instead you can add the [[Winswitch|winswitch]]-repository to your package list.

step 1: starting an XPRA-server at Remeis

First establish a SSH-connection to your favourite machine on Remeis:
<pre>
you@local:~> ssh constellation.sternwarte.uni-erlangen.de
</pre>
Now start an XPRA-server using
<pre>
username@constellation:~> xpra start :123
</pre>
The :123 is an arbitrary display port which any X program will use in a minute. Please note that :0 is reserved for the physical display on your remote desk! To ensure that all X programs will use the XPRA-server you need to modify the DISPLAY environmental variable. In a [[TcShell|CSH]], you can use
<pre>
username@constellation:~> setenv DISPLAY :123
</pre>

step 2: connecting to the XPRA-server

Finally, to display all X program on your local machine, open a new shell and attach the XPRA-session:
<pre>
you@local:~> xpra attach ssh:constellation.sternwarte.uni-erlangen.de:123
</pre>
Here, :123 is again the display port XPRA is using. Any X program or window you start in the SSH-connection will open at your local machine. This work even for plot windows in, e.g., ISIS.

step 2+N: open more SSH connections

Once you need N more terminals on the remeis machines, but still want to forward their X windows to your local machine, just start another SSH-connection and set the DISPLAY variable:
<pre>
you@local:~> ssh constellation.sternwarte.uni-erlangen.de
username@constellation:~> setenv DISPLAY :123
</pre>

final step: shutting down the XPRA-server

If your done with your work you should stop the XPRA-server to free the display port:
<pre>
username@constellation:~> xpra stop :123
</pre>

XPRA and SSH

2018-04-11T14:22:38Z

Sokolova-lapa: Created page with " Category:Working Remotely = Working remotely using XPRA and SSH = [https://www.xpra.org/ XPRA] allows you to start remote X programs and display them on your local mac..."

[[Category:Working Remotely]]

= Working remotely using XPRA and SSH =

[https://www.xpra.org/ XPRA] allows you to start remote X programs and display them on your local machine. [[Winswitch|Winswitch]] uses XPRA internally, but you can use it directly as well. Especially, you can use the speed of [[SSH|SSH]] for commands, but don't need to use X11-forwarding during your SSH-connection, which can be very slow.

First, you need to install XPRA on your local machine. If you are using a Debian-based UNIX-system you can get XPRA via
<pre>
sudo apt-get install xpra
</pre>
Please note that you might not get the current version of XPRA depending on your distribution. Instead you can add the [[Winswitch|winswitch]]-repository to your package list.

step 1: starting an XPRA-server at Remeis

First establish a SSH-connection to your favourite machine on Remeis:
<pre>
you@local:~> ssh constellation.sternwarte.uni-erlangen.de
</pre>
Now start an XPRA-server using
<pre>
username@constellation:~> xpra start :123
</pre>
The :123 is an arbitrary display port which any X program will use in a minute. Please note that :0 is reserved for the physical display on your remote desk! To ensure that all X programs will use the XPRA-server you need to modify the DISPLAY environmental variable. In a [[csh:start|CSH]], you can use
<pre>
username@constellation:~> setenv DISPLAY :123
</pre>

step 2: connecting to the XPRA-server

Finally, to display all X program on your local machine, open a new shell and attach the XPRA-session:
<pre>
you@local:~> xpra attach ssh:constellation.sternwarte.uni-erlangen.de:123
</pre>
Here, :123 is again the display port XPRA is using. Any X program or window you start in the SSH-connection will open at your local machine. This work even for plot windows in, e.g., ISIS.

step 2+N: open more SSH connections

Once you need N more terminals on the remeis machines, but still want to forward their X windows to your local machine, just start another SSH-connection and set the DISPLAY variable:
<pre>
you@local:~> ssh constellation.sternwarte.uni-erlangen.de
username@constellation:~> setenv DISPLAY :123
</pre>

final step: shutting down the XPRA-server

If your done with your work you should stop the XPRA-server to free the display port:
<pre>
username@constellation:~> xpra stop :123
</pre>

Winswitch

2018-04-11T14:12:05Z

Sokolova-lapa: Created page with " Category:Working Remotely = Working remotely using winswitch = The following short guide how to use winswitch is a copy of an email by Thomas Dauser. Since winswitc..."

[[Category:Working Remotely]]

= Working remotely using winswitch =

The following short guide how to use winswitch is a copy of an email by Thomas Dauser. Since winswitch uses XPRA internally, you might use a combination of [[XPRA and SSH|XPRA and SSH]] as well to work remotely.

Winswitch can be simply installed on any system (Linux, Mac, Windows).
Please follow the instructions on their webapge:
[[https://winswitch.org/downloads/]] 
The application is then best started from the graphical launcher.

-------

Instructions for connecting:

1) Just go to the drop-down menu and select "new connection". Add the
infos for your user and host you want to connect to (e.g., your machine
or simply leo.sternwarte.uni-erlangen.de).

2) When you are connected, you are able to start an "Application" and a
"Desktop". Now here comes the major difference:

We do not support a full desktop connection any more!

Instead, what you do, you choose from the drop-down menu:
"Start Application → System → XTerm"

3) A small window opens. You can start any remote graphical application
from this window on the host you are connected to.

=== Problems and helpful Notes ===

* The local server which gets installed with winswitch on your laptop might cause problems (e.g., a strange screen lock behaviour). You should be able to deactivate and still connect to the Remeis cluster.

SSH

2018-04-11T14:02:11Z

Sokolova-lapa:

[[Category:Working Remotely]]

= Working remotely using SSH =

If you want to connect to a machine at Remeis from remote you can use, e.g., SSH. This is a secured connection, which forwards a shell on the machine to your local computer.

=== Linux ===

On a linux system, you need to have SSH installed. On Debian based system, such as Ubuntu, that can be achieved by
<pre>
sudo apt-get install ssh
</pre>
Once SSH is installed, just type
<pre>
ssh username@constellation.sternwarte.uni-erlangen.de
</pre>
into your local shell. Replace username by your login at Remeis and constellation by the name of the machine at Remeis, e.g., leo. You will be then asked by your password. You may use [[SSH-Keys|SSH-Keys]] to avoid entering you password.

It is also possible to enabled X11 forwarding with the -X option, which allows you to open window-based applications, such as konqueror or pgplot:
<pre>
ssh -X username@constellation.sternwarte.uni-erlangen.de
</pre>
In that case the window opens at your local machine. Be aware that X11 forwarding requires a lot of bandwidth, which will slow down the windows and any actions you do significantly. To slightly increase the speed you can choose to compress the commands between bots machines via
<pre>
ssh -X -C username@constellation.sternwarte.uni-erlangen.de
</pre>

==== SSH-Keys ====

To avoid typing in your password at the remove machine every time you log in, you might consider installing [[SSH-Keys|SSH-Keys]].

==== Screen ====

Sometimes, a ssh session will terminate due to the error "Write failed: broken pipe" or something similar.
As this can have various reasons, the best is to use <code>screen</code> in any case.
This allows you to attach and detach a running remote terminal session at any time.
This way, you can run a job on screen, detach the session, switch off the laptop, and resume this remote session later.

To start the screen session type
<pre>
screen
</pre>
To detach it:
<pre>
Cntr-a-d
</pre>
To resume it later:
<pre>
screen -r -d
</pre>

The only disadvantage (unable to scroll back) is no, if you add this to your ~/.screenrc:
<pre>
termcapinfo xterm ti@:te@
termcapinfo xterm-color ti@:te@
</pre>

=== Windows ===

If your local computer is running Windows as operating system you need to download and install a SSH-client, such as [[http://www.putty.org/ PuTTY]]. A guide how to use Putty is available here:
[[http://the.earth.li/~sgtatham/putty/0.64/htmldoc/Chapter2.html#gs]]

SSH

2018-04-11T14:00:20Z

Sokolova-lapa: Created page with " Category:Working Remotely = Working remotely using SSH = If you want to connect to a machine at Remeis from remote you can use, e.g., SSH. This is a secured connection..."

[[Category:Working Remotely]]

= Working remotely using SSH =

If you want to connect to a machine at Remeis from remote you can use, e.g., SSH. This is a secured connection, which forwards a shell on the machine to your local computer.

=== Linux ===

On a linux system, you need to have SSH installed. On Debian based system, such as Ubuntu, that can be achieved by
<pre>
sudo apt-get install ssh
</pre>
Once SSH is installed, just type
<pre>
ssh username@constellation.sternwarte.uni-erlangen.de
</pre>
into your local shell. Replace username by your login at Remeis and constellation by the name of the machine at Remeis, e.g., leo. You will be then asked by your password. You may use [[SSH-Keys|SSH-Keys]] to avoid entering you password.

It is also possible to enabled X11 forwarding with the -X option, which allows you to open window-based applications, such as konqueror or pgplot:
<pre>
ssh -X username@constellation.sternwarte.uni-erlangen.de
</pre>
In that case the window opens at your local machine. Be aware that X11 forwarding requires a lot of bandwidth, which will slow down the windows and any actions you do significantly. To slightly increase the speed you can choose to compress the commands between bots machines via
<pre>
ssh -X -C username@constellation.sternwarte.uni-erlangen.de
</pre>

==== SSH-Keys ====

To avoid typing in your password at the remove machine every time you log in, you might consider installing [[SSH-Keys|SSH-Keys]].

==== Screen ====

Sometimes, a ssh session will terminate due to the error "Write failed: broken pipe" or something similar.
As this can have various reasons, the best is to use <code>screen</code> in any case.
This allows you to attach and detach a running remote terminal session at any time.
This way, you can run a job on screen, detach the session, switch off the laptop, and resume this remote session later.

To start the screen session type
<pre>
screen
</pre>
To detach it:
<pre>
Cntr-a-d
</pre>
To resume it later:
<pre>
screen -r -d
</pre>

The only disadvantage (unable to scroll back) is no, if you add this to your ~/.screenrc:
<pre>
termcapinfo xterm ti@:te@
termcapinfo xterm-color ti@:te@
</pre>

=== Windows ===

If your local computer is running Windows as operating system you need to download and install a SSH-client, such as [[http://www.putty.org/|PuTTY]]. A guide how to use Putty is available here:
[[http://the.earth.li/~sgtatham/putty/0.64/htmldoc/Chapter2.html#gs]]

Trouble shooting

2018-04-11T13:43:04Z

Sokolova-lapa:

[[Category:Trouble Shooting]]

=X-ray satellite data extraction=

===xisextract===
problem: <code>Can't locate common_functions.pm in @INC (@INC contains: /data/system/software/headas/heasoft-6.13/</code> 
solution: common_functions.pn are useful functions used by xisextract and originate in XMM's science analysis software (SAS) that has to be sourced via <code>source $SOFTDIR/sas_init.csh</code>

===xmmprepare / xmmextract===
problem: <code>No eventfile found in /home/user/.../obsid/pn/raw -- aborting</code> 
solution: In some cases an Observational Data File (ODF) is split into more than one observation which makes our scripts fail. See [http://www.mpe.mpg.de/xray/wave/xmm/cookbook/EPIC_PN/merge_odf.php] for the solution!!
And never forget to source $SOFTDIR/sas_init.csh!

=ISIS=

===fits_save_fit ===
problem: <code>fits_save_fit</code> writes too long string (exceeding allowed ASCII length) especially in case of many loaded datasets 
solution: internally, <code>fits_save_fit</code> gets the binning infos from <code>get_data_info(idx).rebin</code> and converts it to a human readable string stating each interval that is binned differently. In case of a simple <code>rebin_data</code> or <code>group</code> command on the current grid, that will create a huge string as every bin of the current grid will be rebinned separately. You can avoid that by defining a custom grid (example by Matthias Kuehnel):
<pre>
(eb,)=log_grid(.5,10,5); % energy grid (.5-10 keV, 5 bins)
mc = int(sqrt(eb*100)); % number of channels in each energy bin (factor 100 somehow is the binning "strength")
group(all_data; min_chan = mc, bounds = eb, unit = "kev");
</pre>
The resulting string will now only have 5 stated intervals

=Firmware 50cm Telescope=
problem: Pointing in RA is very bad 
solution: Check if the time, set in the Handpad, is still correct. The built-in quartz-clock isn't accurate at all and a time difference of up to 30sec in two weeks is possible. I recommend the website "uhrzeit.org" to get the right time. Please note, that the Handpad is still set (and will stay set) to "Daylight Saving" 

problem: startrails, even with short exposure times 
solution: It seems that the tracking speed of the mount has a temperature dependance. Especially at cold temperatures, the normal speed ist no longer accurate enough. A coorection factor can be set in the Handpad (DRIVE → Tracking cor.). To calculate the correction factor one has to take an exposure with startrails (dual tracking off) and calculate the difference between the normal tracking speed an the speed the mount uses. For this purpose, a Python3 programm is available (Schindewolf).

=Guiding with the 50cm Telescope=
Always use a crossover ST4 cable for guiding the 10Micron mount with the ST-i Guider or the internal guiding chip of the STX. As the internal wiring of the ST4 ports of camera and mount is different, a normal ST4 cable could cause trouble. With a crossover cable, the correct pins are connected with each other!
The cable in the St-i case is crossover for example. If you are unsure theck the coloring of the pins, visible through the clear connector.

=CCD Ops=
problem: Ghost images on darks or flats with the STX 16803 
solution: The Ghost images are caused by the architecture of the CCD (Fullframe). They occur when electrons are not "moved away/deleted" after the readout but stay in the pixel. One possibilityis to wait about 10-20 min or do a "NIR-Preflash" (NIR=Near Infrared). This option can be found in the Camera Menu → STX → properties.
But be careful: Once you use it for one picture, you have to use it for every picture of one night. Otherwise the darks and flats would not work correctly anymore as the value of the noise and the response of the pixel changes.

Trouble shooting

2018-04-11T13:32:41Z

Sokolova-lapa:

[[Category:Trouble Shooting]]

=X-ray satellite data extraction=

===xisextract===
problem: <code>Can't locate common_functions.pm in @INC (@INC contains: /data/system/software/headas/heasoft-6.13/</code> 
solution: common_functions.pn are useful functions used by xisextract and originate in XMM's science analysis software (SAS) that has to be sourced via <code>source $SOFTDIR/sas_init.csh</code>
 
===xmmprepare / xmmextract===
problem: <code>No eventfile found in /home/user/.../obsid/pn/raw -- aborting</code> 
solution: In some cases an Observational Data File (ODF) is split into more than one observation which makes our scripts fail. See [http://www.mpe.mpg.de/xray/wave/xmm/cookbook/EPIC_PN/merge_odf.php] for the solution!!
And never forget to source $SOFTDIR/sas_init.csh!

=====ISIS=====

==== fits_save_fit ====
problem: ''fits_save_fit'' writes too long string (exceeding allowed ASCII length) especially in case of many loaded datasets\\
solution: internally, ''fits_save_fit'' gets the binning infos from ''get_data_info(idx).rebin'' and converts it to a human readable string stating each interval that is binned differently. In case of a simple ''rebin_data'' or ''group'' command on the current grid, that will create a huge string as every bin of the current grid will be rebinned separately. You can avoid that by defining a custom grid (example by Matthias Kuehnel):
<pre>
(eb,)=log_grid(.5,10,5); % energy grid (.5-10 keV, 5 bins)
mc = int(sqrt(eb*100)); % number of channels in each energy bin (factor 100 somehow is the binning "strength")
group(all_data; min_chan = mc, bounds = eb, unit = "kev");
</pre>
The resulting string will now only have 5 stated intervals
 
=====Firmware 50cm Telescope=====
problem: Pointing in RA is very bad 
solution: Check if the time, set in the Handpad, is still correct. The built-in quartz-clock isn't accurate at all and a time difference of up to 30sec in two weeks is possible. I recommend the website "uhrzeit.org" to get the right time. Please note, that the Handpad is still set (and will stay set) to "Daylight Saving" 

problem: startrails, even with short exposure times 
solution: It seems that the tracking speed of the mount has a temperature dependance. Especially at cold temperatures, the normal speed ist no longer accurate enough. A coorection factor can be set in the Handpad (DRIVE->Tracking cor.). To calculate the correction factor one has to take an exposure with startrails (dual tracking off) and calculate the difference between the normal tracking speed an the speed the mount uses. For this purpose, a Python3 programm is available (Schindewolf).
 
=====Guiding with the 50cm Telescope=====
Always use a crossover ST4 cable for guiding the 10Micron mount with the ST-i Guider or the internal guiding chip of the STX. As the internal wiring of the ST4 ports of camera and mount is different, a normal ST4 cable could cause trouble. With a crossover cable, the correct pins are connected with each other!
The cable in the St-i case is crossover for example. If you are unsure theck the coloring of the pins, visible through the clear connector.
 
=====CCD Ops=====
problem: Ghost images on darks or flats with the STX 16803\\
solution: The Ghost images are caused by the architecture of the CCD (Fullframe). They occur when electrons are not "moved away/deleted" after the readout but stay in the pixel. One possibilityis to wait about 10-20 min or do a "NIR-Preflash" (NIR=Near Infrared). This option can be found in the Camera Menu &rarr STX &rarr properties.
But be careful: Once you use it for one picture, you have to use it for every picture of one night. Otherwise the darks and flats would not work correctly anymore as the value of the noise and the response of the pixel changes

Trouble shooting

2018-04-11T13:00:27Z

Sokolova-lapa:

[[Category:Trouble Shooting]]

===== X-ray satellite data extraction =====

==== xisextract ====
problem: <code>Can't locate common_functions.pm in @INC (@INC contains: /data/system/software/headas/heasoft-6.13/</code>
solution: common_functions.pn are useful functions used by xisextract and originate in XMM's science analysis software (SAS) that has to be sourced via ''source $SOFTDIR/sas_init.csh''

==== xmmprepare / xmmextract ====
problem: ''No eventfile found in /home/user/.../obsid/pn/raw -- aborting''\\
solution: In some cases an Observational Data File (ODF) is split into more than one observation which makes our scripts fail. See http://www.mpe.mpg.de/xray/wave/xmm/cookbook/EPIC_PN/merge_odf.php for the solution!!
And never forget to source $SOFTDIR/sas_init.csh!
===== ISIS =====

==== fits_save_fit ====
problem: ''fits_save_fit'' writes too long string (exceeding allowed ASCII length) especially in case of many loaded datasets\\
solution: internally, ''fits_save_fit'' gets the binning infos from ''get_data_info(idx).rebin'' and converts it to a human readable string stating each interval that is binned differently. In case of a simple ''rebin_data'' or ''group'' command on the current grid, that will create a huge string as every bin of the current grid will be rebinned separately. You can avoid that by defining a custom grid (example by Matthias Kuehnel):
<code>(eb,)=log_grid(.5,10,5); % energy grid (.5-10 keV, 5 bins)
mc = int(sqrt(eb*100)); % number of channels in each energy bin (factor 100 somehow is the binning "strength")
group(all_data; min_chan = mc, bounds = eb, unit = "kev");</code>
The resulting string will now only have 5 stated intervals

=====Firmware 50cm Telescope=====
problem: Pointing in RA is very bad\\
solution: Check if the time, set in the Handpad, is still correct. The built-in quartz-clock isn't accurate at all and a time difference of up to 30sec in two weeks is possible. I recommend the website "uhrzeit.org" to get the right time. Please note, that the Handpad is still set (and will stay set) to "Daylight Saving"\\
\\
problem: startrails, even with short exposure times\\
solution: It seems that the tracking speed of the mount has a temperature dependance. Especially at cold temperatures, the normal speed ist no longer accurate enough. A coorection factor can be set in the Handpad (DRIVE->Tracking cor.). To calculate the correction factor one has to take an exposure with startrails (dual tracking off) and calculate the difference between the normal tracking speed an the speed the mount uses. For this purpose, a Python3 programm is available (Schindewolf).

=====Guiding with the 50cm Telescope=====
Always use a crossover ST4 cable for guiding the 10Micron mount with the ST-i Guider or the internal guiding chip of the STX. As the internal wiring of the ST4 ports of camera and mount is different, a normal ST4 cable could cause trouble. With a crossover cable, the correct pins are connected with each other!
The cable in the St-i case is crossover for example. If you are unsure theck the coloring of the pins, visible through the clear connector.

=====CCD Ops=====
problem: Ghost images on darks or flats with the STX 16803\\
solution: The Ghost images are caused by the architecture of the CCD (Fullframe). They occur when electrons are not "moved away/deleted" after the readout but stay in the pixel. One possibilityis to wait about 10-20 min or do a "NIR-Preflash" (NIR=Near Infrared). This option can be found in the Camera Menu -> STX -> properties.
But be careful: Once you use it for one picture, you have to use it for every picture of one night. Otherwise the darks and flats would not work correctly anymore as the value of the noise and the response of the pixel changes

Trouble shooting

2018-04-11T12:46:34Z

Sokolova-lapa: Created page with " Category:Trouble Shooting ===== X-ray satellite data extraction ===== ==== xisextract ==== **problem:** ''Can't locate common_functions.pm in @INC (@INC contains: /d..."

[[Category:Trouble Shooting]]

===== X-ray satellite data extraction =====

==== xisextract ====
**problem:** ''Can't locate common_functions.pm in @INC (@INC contains:
/data/system/software/headas/heasoft-6.13/''\\
**solution:** common_functions.pn are useful functions used by xisextract and originate in XMM's science analysis software (SAS) that has to be sourced via ''source $SOFTDIR/sas_init.csh''

==== xmmprepare / xmmextract ====
**problem:** ''No eventfile found in /home/user/.../obsid/pn/raw -- aborting''\\
**solution:** In some cases an Observational Data File (ODF) is split into more than one observation which makes our scripts fail. See http://www.mpe.mpg.de/xray/wave/xmm/cookbook/EPIC_PN/merge_odf.php for the solution!!
And never forget to source $SOFTDIR/sas_init.csh!
===== ISIS =====

==== fits_save_fit ====
**problem:** ''fits_save_fit'' writes too long string (exceeding allowed ASCII length) especially in case of many loaded datasets\\
**solution:** internally, ''fits_save_fit'' gets the binning infos from ''get_data_info(idx).rebin'' and converts it to a human readable string stating each interval that is binned differently. In case of a simple ''rebin_data'' or ''group'' command on the current grid, that will create a huge string as every bin of the current grid will be rebinned separately. You can avoid that by defining a custom grid (example by Matthias Kuehnel):
<code>(eb,)=log_grid(.5,10,5); % energy grid (.5-10 keV, 5 bins)
mc = int(sqrt(eb*100)); % number of channels in each energy bin (factor 100 somehow is the binning "strength")
group(all_data; min_chan = mc, bounds = eb, unit = "kev");</code>
The resulting string will now only have 5 stated intervals

=====Firmware 50cm Telescope=====
**problem:** Pointing in RA is very bad\\
**solution:** Check if the time, set in the Handpad, is still correct. The built-in quartz-clock isn't accurate at all and a time difference of up to 30sec in two weeks is possible. I recommend the website "uhrzeit.org" to get the right time. Please note, that the Handpad is still set (and will stay set) to "Daylight Saving"\\
\\
**problem:** startrails, even with short exposure times\\
**solution:** It seems that the tracking speed of the mount has a temperature dependance. Especially at cold temperatures, the normal speed ist no longer accurate enough. A coorection factor can be set in the Handpad (DRIVE->Tracking cor.). To calculate the correction factor one has to take an exposure with startrails (dual tracking off) and calculate the difference between the normal tracking speed an the speed the mount uses. For this purpose, a Python3 programm is available (Schindewolf).

=====Guiding with the 50cm Telescope=====
Always use a crossover ST4 cable for guiding the 10Micron mount with the ST-i Guider or the internal guiding chip of the STX. As the internal wiring of the ST4 ports of camera and mount is different, a normal ST4 cable could cause trouble. With a crossover cable, the correct pins are connected with each other!
The cable in the St-i case is crossover for example. If you are unsure theck the coloring of the pins, visible through the clear connector.

=====CCD Ops=====
**problem:** Ghost images on darks or flats with the STX 16803\\
**solution:** The Ghost images are caused by the architecture of the CCD (Fullframe). They occur when electrons are not "moved away/deleted" after the readout but stay in the pixel. One possibilityis to wait about 10-20 min or do a "NIR-Preflash" (NIR=Near Infrared). This option can be found in the Camera Menu -> STX -> properties.
But be careful: Once you use it for one picture, you have to use it for every picture of one night. Otherwise the darks and flats would not work correctly anymore as the value of the noise and the response of the pixel changes