Remeis-Wiki - User contributions [en]

File:PP Shtykovsky 2017 Fig1.png

2023-09-16T14:31:26Z

Kretschmar: /* Summary */

== Summary ==
LMC X-4: NuSTAR profiles in different energy bands

LMC X-4

2023-09-07T09:09:36Z

Kretschmar: /* Observed pulse profiles */ Added Shtykovsky et al. (2017)

[[Category:Accreting X-ray Pulsars]]

= Other Names =

3A 0529-660

= Observed pulse profiles =

<gallery mode=packed heights=240px >
File:PP Alonso-Hernandez 2022 FigA21.png | [https://ui.adsabs.harvard.edu/abs/2020A%2526A...638A.152R/abstract Alonso-Hernández et al. (2022)]: XMM-Newton pulse profiles at different luminosities
File:PP Alonso-Hernandez 2022 FigA22.png | [https://ui.adsabs.harvard.edu/abs/2020A%2526A...638A.152R/abstract Alonso-Hernández et al. (2022)]: NuSTAR pulse profiles at different luminosities
File:PP Brumback2018 Fig3.png | [https://ui.adsabs.harvard.edu/abs/2018ApJ...861L...7B/abstract Brumback et al. (2018)]: NuSTAR pulse profiles during one observation
File:PP Shtykovsky 2018 Fig3.png | [https://ui.adsabs.harvard.edu/abs/2018AstL...44..149S/abstract Shtykovsky et al. (2018)]
File:PP Shtykovsky 2018 Fig4.png | [https://ui.adsabs.harvard.edu/abs/2018AstL...44..149S/abstract Shtykovsky et al. (2018)]
File:PP Shtykovsky 2018 Fig5.png | [https://ui.adsabs.harvard.edu/abs/2018AstL...44..149S/abstract Shtykovsky et al. (2018)]
File:PP Shtykovsky 2018 Fig6.png | [https://ui.adsabs.harvard.edu/abs/2018AstL...44..149S/abstract Shtykovsky et al. (2018)]
File:PP Shtykovsky 2017 Fig1.png | [https://ui.adsabs.harvard.edu/abs/2017AstL...43..175S/abstract Shtykovsky et al. (2017)]
</gallery>

File:PP Shtykovsky 2018 Fig1.png

2023-09-07T09:08:08Z

Kretschmar: Kretschmar moved page File:PP Shtykovsky 2018 Fig1.png to File:PP Shtykovsky 2017 Fig1.png: Wrong p

#REDIRECT [[File:PP Shtykovsky 2017 Fig1.png]]

File:PP Shtykovsky 2017 Fig1.png

2023-09-07T09:08:08Z

Kretschmar: Kretschmar moved page File:PP Shtykovsky 2018 Fig1.png to File:PP Shtykovsky 2017 Fig1.png: Wrong p

== Summary ==
NuSTAR profiles in different energy bands

File:PP Shtykovsky 2017 Fig1.png

2023-09-07T09:05:20Z

Kretschmar: NuSTAR profiles in different energy bands

== Summary ==
NuSTAR profiles in different energy bands

LMC X-4

2023-09-07T08:59:40Z

Kretschmar: Added pulse profles from Shtykovsky et al. (2018)

File:PP Shtykovsky 2018 Fig6.png

2023-09-07T08:35:21Z

Kretschmar: More profiles including intervals with stars.

== Summary ==
More profiles including intervals with stars.

File:PP Shtykovsky 2018 Fig5.png

2023-09-07T08:32:45Z

Kretschmar: Further profiles of selected intervals, with times containing flares marked by stars.

== Summary ==
Further profiles of selected intervals, with times containing flares marked by stars.

File:PP Shtykovsky 2018 Fig4.png

2023-09-07T08:30:33Z

Kretschmar: Pulse profiles from different intervals, those with flares marked by a star.

== Summary ==
Pulse profiles from different intervals, those with flares marked by a star.

File:PP Shtykovsky 2018 Fig3.png

2023-09-06T21:49:40Z

Kretschmar: Pulse profiles at low luminosity

== Summary ==
Pulse profiles at low luminosity

LMC X-4

2023-09-06T21:44:48Z

Kretschmar:

File:PP Brumback2018 Fig3.png

2023-09-06T21:42:15Z

Kretschmar: NuSTAR pulse profiles from one observation including a flare.

== Summary ==
NuSTAR pulse profiles from one observation including a flare.

LMC X-4

2023-09-06T21:37:09Z

Kretschmar: Start pulse profile gallery

File:PP Alonso-Hernandez 2022 FigA22.png

2023-09-06T21:27:48Z

Kretschmar: NuSTAR profiles

== Summary ==
NuSTAR profiles

File:PP Alonso-Hernandez 2022 FigA21.png

2023-09-06T21:25:04Z

Kretschmar: XMM-Newton profiles

== Summary ==
XMM-Newton profiles

V 0332+53

2023-09-06T21:08:12Z

Kretschmar: /* Observed pulse profiles */

[[Category:Accreting X-ray Pulsars]]

Also known as EXO 0331+530 and V BQ Cam [http://simbad.u-strasbg.fr/simbad/sim-id?Ident=V0332%2B53&NbIdent=1&Radius=2&Radius.unit=arcmin&submit=submit+id Simbad] <ref name="Tanaka83" /> <ref name="Makishima90b" />

'''Monitoring Data''':

[http://xte.mit.edu/asmlc/srcs/v0332+53.html RXTE/ASM]
[http://swift.gsfc.nasa.gov/docs/swift/results/transients/V0332p53 Swift/BAT]
[http://maxi.riken.jp/top/index.php?cid=1&jname=J0334+531 MAXI]
[http://gammaray.nsstc.nasa.gov/gbm/science/pulsars/lightcurves/v0332.html Fermi/GBM pulsed flux]
[http://integral.esac.esa.int/flashes-plots/EXO%200331+530_plot.html Current data in FLASHES]

= System Overview =

{| class="wikitable"
|Porb
| 34.25
| days
| <ref name="Stella85" />
|-
|Pspin
| ~4.4
| s
| <ref name="Stella85" />
|-
|B
| 2.7 x 1012
| G
| <ref name="Pottschmidt05" />
|-
|a sin i
| 48±4
| lt-sec
| <ref name="Stella85" />
|-
|eccentricity
| 0.31±0.03
|
| <ref name="Stella85" />
|-
|ω
| 313±10
|degree
| <ref name="Stella85" />
|-
|Τperiastron
| 2445652±1
| JD
| <ref name="Stella85" />
|-
|distance
| ~7
| kpc
| <ref name="Negueruela99" />
|}

= Description =

V 0332+53 was first recognized in Tenma observations from late 1983 to January 1984
(<ref name="Tanaka83" />, <ref name="Makishima90b" />). After the detection it was realized that it had been seen by Vela 5B in 1973
(<ref name="TerrellPriedhorsky84" />). Follow-up observations by EXOSAT discovered pulsations and allowed the determination of orbital parameters (<ref name="Stella85" />).

The Tenma observations already showed evidence for a cyclotron line at ~28 keV.
Ginga observations (2–60 keV) during an outburst in 1989 found two lines at 28.5 and 53 keV (<ref name="Makishima90" />). During the next bright outburst in 2004, INTEGRAL observations (<ref name="Pottschmidt05" />) found a third cyclotron line at ~74 keV.

= Observed pulse profiles =

<gallery mode=packed heights=240px >
File:PP_AH2022_V0332%2B53_Fig7.png|[https://ui.adsabs.harvard.edu/abs/2020A%2526A...638A.152R/abstract Alonso-Hernández et al. (2022)]: NuSTAR pulse profiles at different luminosities
File:PP_Bykov21_V0332%2B53.png | [https://ui.adsabs.harvard.edu/abs/2021MNRAS.506.2156B/abstract Bykov et al. (2021)] RXTE/PCA data
File:PP_Sasaki2012_Fig5.png | [https://ui.adsabs.harvard.edu/abs/2012A%26A...540A..35S/abstract Sasaki et al. (2012)] RXTE data
File:PP_Tsygankov2006_Fig6.png | [https://ui.adsabs.harvard.edu/abs/2006MNRAS.371...19T/abstract Tsygankov et al. (2006)] INTEGRAL JEM-X and IBIS
File:PP_Zhang2005_Fig3.png | [https://ui.adsabs.harvard.edu/abs/2005ApJ...630L..65Z/abstract Zhang et al. (2005)] RXTE PCA and INTEGRAL
File:PP_Stella1985_Fig1.png | [https://ui.adsabs.harvard.edu/abs/1985ApJ...288L..45S/abstract Stella et al. (1985)] EXOSAT
</gallery>

= Bibliography =
'''References'''

File:PP Stella1985 Fig1.png

2023-09-06T21:06:51Z

Kretschmar: Power spectra and pulse profiles for V0332+53 on two different dates

== Summary ==
Power spectra and pulse profiles for V0332+53 on two different dates

V 0332+53

2023-09-05T14:18:10Z

Kretschmar: /* Observed pulse profiles */

V 0332+53

2023-09-05T14:17:11Z

Kretschmar: /* Observed pulse profiles */

[[Category:Accreting X-ray Pulsars]]

Also known as EXO 0331+530 and V BQ Cam [http://simbad.u-strasbg.fr/simbad/sim-id?Ident=V0332%2B53&NbIdent=1&Radius=2&Radius.unit=arcmin&submit=submit+id Simbad] <ref name="Tanaka83" /> <ref name="Makishima90b" />

'''Monitoring Data''':

[http://xte.mit.edu/asmlc/srcs/v0332+53.html RXTE/ASM]
[http://swift.gsfc.nasa.gov/docs/swift/results/transients/V0332p53 Swift/BAT]
[http://maxi.riken.jp/top/index.php?cid=1&jname=J0334+531 MAXI]
[http://gammaray.nsstc.nasa.gov/gbm/science/pulsars/lightcurves/v0332.html Fermi/GBM pulsed flux]
[http://integral.esac.esa.int/flashes-plots/EXO%200331+530_plot.html Current data in FLASHES]

= System Overview =

{| class="wikitable"
|Porb
| 34.25
| days
| <ref name="Stella85" />
|-
|Pspin
| ~4.4
| s
| <ref name="Stella85" />
|-
|B
| 2.7 x 1012
| G
| <ref name="Pottschmidt05" />
|-
|a sin i
| 48±4
| lt-sec
| <ref name="Stella85" />
|-
|eccentricity
| 0.31±0.03
|
| <ref name="Stella85" />
|-
|ω
| 313±10
|degree
| <ref name="Stella85" />
|-
|Τperiastron
| 2445652±1
| JD
| <ref name="Stella85" />
|-
|distance
| ~7
| kpc
| <ref name="Negueruela99" />
|}

= Description =

V 0332+53 was first recognized in Tenma observations from late 1983 to January 1984
(<ref name="Tanaka83" />, <ref name="Makishima90b" />). After the detection it was realized that it had been seen by Vela 5B in 1973
(<ref name="TerrellPriedhorsky84" />). Follow-up observations by EXOSAT discovered pulsations and allowed the determination of orbital parameters (<ref name="Stella85" />).

The Tenma observations already showed evidence for a cyclotron line at ~28 keV.
Ginga observations (2–60 keV) during an outburst in 1989 found two lines at 28.5 and 53 keV (<ref name="Makishima90" />). During the next bright outburst in 2004, INTEGRAL observations (<ref name="Pottschmidt05" />) found a third cyclotron line at ~74 keV.

= Observed pulse profiles =

<gallery mode=packed heights=300px >
File:PP_AH2022_V0332%2B53_Fig7.png|[https://ui.adsabs.harvard.edu/abs/2020A%2526A...638A.152R/abstract Alonso-Hernández et al. (2022)]: NuSTAR pulse profiles at different luminosities
File:PP_Bykov21_V0332%2B53.png | [https://ui.adsabs.harvard.edu/abs/2021MNRAS.506.2156B/abstract Bykov et al. (2021)] RXTE/PCA data
File:PP_Sasaki2012_Fig5.png | [https://ui.adsabs.harvard.edu/abs/2012A%26A...540A..35S/abstract Sasaki et al. (2012)] RXTE data
File:PP_Tsygankov2006_Fig6.png | [https://ui.adsabs.harvard.edu/abs/2006MNRAS.371...19T/abstract Tsygankov et al. (2006)] INTEGRAL JEM-X and IBIS
File:PP_Zhang2005_Fig3.png | [https://ui.adsabs.harvard.edu/abs/2005ApJ...630L..65Z/abstract Zhang et al. (2005)] RXTE PCA and INTEGRAL
</gallery>

= Bibliography =
'''References'''

V 0332+53

2023-09-05T14:16:20Z

Kretschmar: /* Observed pulse profiles */

[[Category:Accreting X-ray Pulsars]]

Also known as EXO 0331+530 and V BQ Cam [http://simbad.u-strasbg.fr/simbad/sim-id?Ident=V0332%2B53&NbIdent=1&Radius=2&Radius.unit=arcmin&submit=submit+id Simbad] <ref name="Tanaka83" /> <ref name="Makishima90b" />

'''Monitoring Data''':

[http://xte.mit.edu/asmlc/srcs/v0332+53.html RXTE/ASM]
[http://swift.gsfc.nasa.gov/docs/swift/results/transients/V0332p53 Swift/BAT]
[http://maxi.riken.jp/top/index.php?cid=1&jname=J0334+531 MAXI]
[http://gammaray.nsstc.nasa.gov/gbm/science/pulsars/lightcurves/v0332.html Fermi/GBM pulsed flux]
[http://integral.esac.esa.int/flashes-plots/EXO%200331+530_plot.html Current data in FLASHES]

= System Overview =

{| class="wikitable"
|Porb
| 34.25
| days
| <ref name="Stella85" />
|-
|Pspin
| ~4.4
| s
| <ref name="Stella85" />
|-
|B
| 2.7 x 1012
| G
| <ref name="Pottschmidt05" />
|-
|a sin i
| 48±4
| lt-sec
| <ref name="Stella85" />
|-
|eccentricity
| 0.31±0.03
|
| <ref name="Stella85" />
|-
|ω
| 313±10
|degree
| <ref name="Stella85" />
|-
|Τperiastron
| 2445652±1
| JD
| <ref name="Stella85" />
|-
|distance
| ~7
| kpc
| <ref name="Negueruela99" />
|}

= Description =

V 0332+53 was first recognized in Tenma observations from late 1983 to January 1984
(<ref name="Tanaka83" />, <ref name="Makishima90b" />). After the detection it was realized that it had been seen by Vela 5B in 1973
(<ref name="TerrellPriedhorsky84" />). Follow-up observations by EXOSAT discovered pulsations and allowed the determination of orbital parameters (<ref name="Stella85" />).

The Tenma observations already showed evidence for a cyclotron line at ~28 keV.
Ginga observations (2–60 keV) during an outburst in 1989 found two lines at 28.5 and 53 keV (<ref name="Makishima90" />). During the next bright outburst in 2004, INTEGRAL observations (<ref name="Pottschmidt05" />) found a third cyclotron line at ~74 keV.

= Observed pulse profiles =

<gallery mode=packed widths=400px >
File:PP_AH2022_V0332%2B53_Fig7.png|[https://ui.adsabs.harvard.edu/abs/2020A%2526A...638A.152R/abstract Alonso-Hernández et al. (2022)]: NuSTAR pulse profiles at different luminosities
File:PP_Bykov21_V0332%2B53.png | [https://ui.adsabs.harvard.edu/abs/2021MNRAS.506.2156B/abstract Bykov et al. (2021)] RXTE/PCA data
File:PP_Sasaki2012_Fig5.png | [https://ui.adsabs.harvard.edu/abs/2012A%26A...540A..35S/abstract Sasaki et al. (2012)] RXTE data
File:PP_Tsygankov2006_Fig6.png | [https://ui.adsabs.harvard.edu/abs/2006MNRAS.371...19T/abstract Tsygankov et al. (2006)] INTEGRAL JEM-X and IBIS
File:PP_Zhang2005_Fig3.png | [https://ui.adsabs.harvard.edu/abs/2005ApJ...630L..65Z/abstract Zhang et al. (2005)] RXTE PCA and INTEGRAL
</gallery>

= Bibliography =
'''References'''

V 0332+53

2023-09-05T14:15:27Z

Kretschmar: /* Observed pulse profiles */

[[Category:Accreting X-ray Pulsars]]

Also known as EXO 0331+530 and V BQ Cam [http://simbad.u-strasbg.fr/simbad/sim-id?Ident=V0332%2B53&NbIdent=1&Radius=2&Radius.unit=arcmin&submit=submit+id Simbad] <ref name="Tanaka83" /> <ref name="Makishima90b" />

'''Monitoring Data''':

[http://xte.mit.edu/asmlc/srcs/v0332+53.html RXTE/ASM]
[http://swift.gsfc.nasa.gov/docs/swift/results/transients/V0332p53 Swift/BAT]
[http://maxi.riken.jp/top/index.php?cid=1&jname=J0334+531 MAXI]
[http://gammaray.nsstc.nasa.gov/gbm/science/pulsars/lightcurves/v0332.html Fermi/GBM pulsed flux]
[http://integral.esac.esa.int/flashes-plots/EXO%200331+530_plot.html Current data in FLASHES]

= System Overview =

{| class="wikitable"
|Porb
| 34.25
| days
| <ref name="Stella85" />
|-
|Pspin
| ~4.4
| s
| <ref name="Stella85" />
|-
|B
| 2.7 x 1012
| G
| <ref name="Pottschmidt05" />
|-
|a sin i
| 48±4
| lt-sec
| <ref name="Stella85" />
|-
|eccentricity
| 0.31±0.03
|
| <ref name="Stella85" />
|-
|ω
| 313±10
|degree
| <ref name="Stella85" />
|-
|Τperiastron
| 2445652±1
| JD
| <ref name="Stella85" />
|-
|distance
| ~7
| kpc
| <ref name="Negueruela99" />
|}

= Description =

V 0332+53 was first recognized in Tenma observations from late 1983 to January 1984
(<ref name="Tanaka83" />, <ref name="Makishima90b" />). After the detection it was realized that it had been seen by Vela 5B in 1973
(<ref name="TerrellPriedhorsky84" />). Follow-up observations by EXOSAT discovered pulsations and allowed the determination of orbital parameters (<ref name="Stella85" />).

The Tenma observations already showed evidence for a cyclotron line at ~28 keV.
Ginga observations (2–60 keV) during an outburst in 1989 found two lines at 28.5 and 53 keV (<ref name="Makishima90" />). During the next bright outburst in 2004, INTEGRAL observations (<ref name="Pottschmidt05" />) found a third cyclotron line at ~74 keV.

= Observed pulse profiles =

<gallery mode=packed>
File:PP_AH2022_V0332%2B53_Fig7.png|[https://ui.adsabs.harvard.edu/abs/2020A%2526A...638A.152R/abstract Alonso-Hernández et al. (2022)]: NuSTAR pulse profiles at different luminosities
File:PP_Bykov21_V0332%2B53.png | [https://ui.adsabs.harvard.edu/abs/2021MNRAS.506.2156B/abstract Bykov et al. (2021)] RXTE/PCA data
File:PP_Sasaki2012_Fig5.png | [https://ui.adsabs.harvard.edu/abs/2012A%26A...540A..35S/abstract Sasaki et al. (2012)] RXTE data
File:PP_Tsygankov2006_Fig6.png | [https://ui.adsabs.harvard.edu/abs/2006MNRAS.371...19T/abstract Tsygankov et al. (2006)] INTEGRAL JEM-X and IBIS
File:PP_Zhang2005_Fig3.png | [https://ui.adsabs.harvard.edu/abs/2005ApJ...630L..65Z/abstract Zhang et al. (2005)] RXTE PCA and INTEGRAL
</gallery>

= Bibliography =
'''References'''

V 0332+53

2023-09-05T14:12:38Z

Kretschmar: /* Observed pulse profiles */

[[Category:Accreting X-ray Pulsars]]

Also known as EXO 0331+530 and V BQ Cam [http://simbad.u-strasbg.fr/simbad/sim-id?Ident=V0332%2B53&NbIdent=1&Radius=2&Radius.unit=arcmin&submit=submit+id Simbad] <ref name="Tanaka83" /> <ref name="Makishima90b" />

'''Monitoring Data''':

[http://xte.mit.edu/asmlc/srcs/v0332+53.html RXTE/ASM]
[http://swift.gsfc.nasa.gov/docs/swift/results/transients/V0332p53 Swift/BAT]
[http://maxi.riken.jp/top/index.php?cid=1&jname=J0334+531 MAXI]
[http://gammaray.nsstc.nasa.gov/gbm/science/pulsars/lightcurves/v0332.html Fermi/GBM pulsed flux]
[http://integral.esac.esa.int/flashes-plots/EXO%200331+530_plot.html Current data in FLASHES]

= System Overview =

{| class="wikitable"
|Porb
| 34.25
| days
| <ref name="Stella85" />
|-
|Pspin
| ~4.4
| s
| <ref name="Stella85" />
|-
|B
| 2.7 x 1012
| G
| <ref name="Pottschmidt05" />
|-
|a sin i
| 48±4
| lt-sec
| <ref name="Stella85" />
|-
|eccentricity
| 0.31±0.03
|
| <ref name="Stella85" />
|-
|ω
| 313±10
|degree
| <ref name="Stella85" />
|-
|Τperiastron
| 2445652±1
| JD
| <ref name="Stella85" />
|-
|distance
| ~7
| kpc
| <ref name="Negueruela99" />
|}

= Description =

V 0332+53 was first recognized in Tenma observations from late 1983 to January 1984
(<ref name="Tanaka83" />, <ref name="Makishima90b" />). After the detection it was realized that it had been seen by Vela 5B in 1973
(<ref name="TerrellPriedhorsky84" />). Follow-up observations by EXOSAT discovered pulsations and allowed the determination of orbital parameters (<ref name="Stella85" />).

The Tenma observations already showed evidence for a cyclotron line at ~28 keV.
Ginga observations (2–60 keV) during an outburst in 1989 found two lines at 28.5 and 53 keV (<ref name="Makishima90" />). During the next bright outburst in 2004, INTEGRAL observations (<ref name="Pottschmidt05" />) found a third cyclotron line at ~74 keV.

= Observed pulse profiles =

<gallery>
File:PP_AH2022_V0332%2B53_Fig7.png|[https://ui.adsabs.harvard.edu/abs/2020A%2526A...638A.152R/abstract Alonso-Hernández et al. (2022)]: NuSTAR pulse profiles at different luminosities
File:PP_Bykov21_V0332%2B53.png | [https://ui.adsabs.harvard.edu/abs/2021MNRAS.506.2156B/abstract Bykov et al. (2021)] RXTE/PCA data
</gallery>

[https://ui.adsabs.harvard.edu/abs/2020A%2526A...638A.152R/abstract Alonso-Hernández et al. (2022)] and with different pulse types. From left to right, LX ≈ 15, 8 and 1 × 1037 erg/s, the first and last have been classified as pulse type 2, the intermediate as type 0.
[[File:PP_AH2022_V0332%2B53_Fig7.png|thumb|right]]

RXTE/PCA data
[[|thumb|right]]

[https://ui.adsabs.harvard.edu/abs/2012A%26A...540A..35S/abstract Sasaki et al. (2012)] RXTE data

[[File:PP_Sasaki2012_Fig5.png|300px]]

[https://ui.adsabs.harvard.edu/abs/2006MNRAS.371...19T/abstract Tsygankov et al. (2006)] INTEGRAL JEM-X and IBIS

[[File:PP_Tsygankov2006_Fig6.png|200px]]

[https://ui.adsabs.harvard.edu/abs/2005ApJ...630L..65Z/abstract Zhang et al. (2005)] RXTE PCA and INTEGRAL

[[File:PP_Zhang2005_Fig3.png|150px]]

= Bibliography =
'''References'''

V 0332+53

2023-09-05T14:10:45Z

Kretschmar: /* Observed pulse profiles */

[[Category:Accreting X-ray Pulsars]]

Also known as EXO 0331+530 and V BQ Cam [http://simbad.u-strasbg.fr/simbad/sim-id?Ident=V0332%2B53&NbIdent=1&Radius=2&Radius.unit=arcmin&submit=submit+id Simbad] <ref name="Tanaka83" /> <ref name="Makishima90b" />

'''Monitoring Data''':

[http://xte.mit.edu/asmlc/srcs/v0332+53.html RXTE/ASM]
[http://swift.gsfc.nasa.gov/docs/swift/results/transients/V0332p53 Swift/BAT]
[http://maxi.riken.jp/top/index.php?cid=1&jname=J0334+531 MAXI]
[http://gammaray.nsstc.nasa.gov/gbm/science/pulsars/lightcurves/v0332.html Fermi/GBM pulsed flux]
[http://integral.esac.esa.int/flashes-plots/EXO%200331+530_plot.html Current data in FLASHES]

= System Overview =

{| class="wikitable"
|Porb
| 34.25
| days
| <ref name="Stella85" />
|-
|Pspin
| ~4.4
| s
| <ref name="Stella85" />
|-
|B
| 2.7 x 1012
| G
| <ref name="Pottschmidt05" />
|-
|a sin i
| 48±4
| lt-sec
| <ref name="Stella85" />
|-
|eccentricity
| 0.31±0.03
|
| <ref name="Stella85" />
|-
|ω
| 313±10
|degree
| <ref name="Stella85" />
|-
|Τperiastron
| 2445652±1
| JD
| <ref name="Stella85" />
|-
|distance
| ~7
| kpc
| <ref name="Negueruela99" />
|}

= Description =

V 0332+53 was first recognized in Tenma observations from late 1983 to January 1984
(<ref name="Tanaka83" />, <ref name="Makishima90b" />). After the detection it was realized that it had been seen by Vela 5B in 1973
(<ref name="TerrellPriedhorsky84" />). Follow-up observations by EXOSAT discovered pulsations and allowed the determination of orbital parameters (<ref name="Stella85" />).

The Tenma observations already showed evidence for a cyclotron line at ~28 keV.
Ginga observations (2–60 keV) during an outburst in 1989 found two lines at 28.5 and 53 keV (<ref name="Makishima90" />). During the next bright outburst in 2004, INTEGRAL observations (<ref name="Pottschmidt05" />) found a third cyclotron line at ~74 keV.

= Observed pulse profiles =

<gallery>
File:PP_AH2022_V0332%2B53_Fig7.png|[https://ui.adsabs.harvard.edu/abs/2020A%2526A...638A.152R/abstract Alonso-Hernández et al. (2022): NuSTAR pulse profiles at different luminosities
File:PP_Bykov21_V0332%2B53.png | RXTE/PCA data
</gallery>

[https://ui.adsabs.harvard.edu/abs/2020A%2526A...638A.152R/abstract Alonso-Hernández et al. (2022)] and with different pulse types. From left to right, LX ≈ 15, 8 and 1 × 1037 erg/s, the first and last have been classified as pulse type 2, the intermediate as type 0.
[[File:PP_AH2022_V0332%2B53_Fig7.png|thumb|right]]

[https://ui.adsabs.harvard.edu/abs/2021MNRAS.506.2156B/abstract Bykov et al. (2021)] RXTE/PCA data
[[|thumb|right]]

[https://ui.adsabs.harvard.edu/abs/2012A%26A...540A..35S/abstract Sasaki et al. (2012)] RXTE data

[[File:PP_Sasaki2012_Fig5.png|300px]]

[https://ui.adsabs.harvard.edu/abs/2006MNRAS.371...19T/abstract Tsygankov et al. (2006)] INTEGRAL JEM-X and IBIS

[[File:PP_Tsygankov2006_Fig6.png|200px]]

[https://ui.adsabs.harvard.edu/abs/2005ApJ...630L..65Z/abstract Zhang et al. (2005)] RXTE PCA and INTEGRAL

[[File:PP_Zhang2005_Fig3.png|150px]]

= Bibliography =
'''References'''

V 0332+53

2023-09-05T14:06:01Z

Kretschmar: /* Observed pulse profiles */

[[Category:Accreting X-ray Pulsars]]

Also known as EXO 0331+530 and V BQ Cam [http://simbad.u-strasbg.fr/simbad/sim-id?Ident=V0332%2B53&NbIdent=1&Radius=2&Radius.unit=arcmin&submit=submit+id Simbad] <ref name="Tanaka83" /> <ref name="Makishima90b" />

'''Monitoring Data''':

[http://xte.mit.edu/asmlc/srcs/v0332+53.html RXTE/ASM]
[http://swift.gsfc.nasa.gov/docs/swift/results/transients/V0332p53 Swift/BAT]
[http://maxi.riken.jp/top/index.php?cid=1&jname=J0334+531 MAXI]
[http://gammaray.nsstc.nasa.gov/gbm/science/pulsars/lightcurves/v0332.html Fermi/GBM pulsed flux]
[http://integral.esac.esa.int/flashes-plots/EXO%200331+530_plot.html Current data in FLASHES]

= System Overview =

{| class="wikitable"
|Porb
| 34.25
| days
| <ref name="Stella85" />
|-
|Pspin
| ~4.4
| s
| <ref name="Stella85" />
|-
|B
| 2.7 x 1012
| G
| <ref name="Pottschmidt05" />
|-
|a sin i
| 48±4
| lt-sec
| <ref name="Stella85" />
|-
|eccentricity
| 0.31±0.03
|
| <ref name="Stella85" />
|-
|ω
| 313±10
|degree
| <ref name="Stella85" />
|-
|Τperiastron
| 2445652±1
| JD
| <ref name="Stella85" />
|-
|distance
| ~7
| kpc
| <ref name="Negueruela99" />
|}

= Description =

V 0332+53 was first recognized in Tenma observations from late 1983 to January 1984
(<ref name="Tanaka83" />, <ref name="Makishima90b" />). After the detection it was realized that it had been seen by Vela 5B in 1973
(<ref name="TerrellPriedhorsky84" />). Follow-up observations by EXOSAT discovered pulsations and allowed the determination of orbital parameters (<ref name="Stella85" />).

The Tenma observations already showed evidence for a cyclotron line at ~28 keV.
Ginga observations (2–60 keV) during an outburst in 1989 found two lines at 28.5 and 53 keV (<ref name="Makishima90" />). During the next bright outburst in 2004, INTEGRAL observations (<ref name="Pottschmidt05" />) found a third cyclotron line at ~74 keV.

= Observed pulse profiles =

[https://ui.adsabs.harvard.edu/abs/2020A%2526A...638A.152R/abstract Alonso-Hernández et al. (2022)] NuSTAR pulse profiles at different luminosities and with different pulse types. From left to right, LX ≈ 15, 8 and 1 × 1037 erg/s, the first and last have been classified as pulse type 2, the intermediate as type 0.
[[File:PP_AH2022_V0332%2B53_Fig7.png|thumb|right]]

[https://ui.adsabs.harvard.edu/abs/2021MNRAS.506.2156B/abstract Bykov et al. (2021)] RXTE/PCA data
[[File:PP_Bykov21_V0332%2B53.png|thumb|right]]

[https://ui.adsabs.harvard.edu/abs/2012A%26A...540A..35S/abstract Sasaki et al. (2012)] RXTE data

[[File:PP_Sasaki2012_Fig5.png|300px]]

[https://ui.adsabs.harvard.edu/abs/2006MNRAS.371...19T/abstract Tsygankov et al. (2006)] INTEGRAL JEM-X and IBIS

[[File:PP_Tsygankov2006_Fig6.png|200px]]

[https://ui.adsabs.harvard.edu/abs/2005ApJ...630L..65Z/abstract Zhang et al. (2005)] RXTE PCA and INTEGRAL

[[File:PP_Zhang2005_Fig3.png|150px]]

= Bibliography =
'''References'''

V 0332+53

2023-09-05T14:05:24Z

Kretschmar: /* Observed pulse profiles */

[[Category:Accreting X-ray Pulsars]]

Also known as EXO 0331+530 and V BQ Cam [http://simbad.u-strasbg.fr/simbad/sim-id?Ident=V0332%2B53&NbIdent=1&Radius=2&Radius.unit=arcmin&submit=submit+id Simbad] <ref name="Tanaka83" /> <ref name="Makishima90b" />

'''Monitoring Data''':

[http://xte.mit.edu/asmlc/srcs/v0332+53.html RXTE/ASM]
[http://swift.gsfc.nasa.gov/docs/swift/results/transients/V0332p53 Swift/BAT]
[http://maxi.riken.jp/top/index.php?cid=1&jname=J0334+531 MAXI]
[http://gammaray.nsstc.nasa.gov/gbm/science/pulsars/lightcurves/v0332.html Fermi/GBM pulsed flux]
[http://integral.esac.esa.int/flashes-plots/EXO%200331+530_plot.html Current data in FLASHES]

= System Overview =

{| class="wikitable"
|Porb
| 34.25
| days
| <ref name="Stella85" />
|-
|Pspin
| ~4.4
| s
| <ref name="Stella85" />
|-
|B
| 2.7 x 1012
| G
| <ref name="Pottschmidt05" />
|-
|a sin i
| 48±4
| lt-sec
| <ref name="Stella85" />
|-
|eccentricity
| 0.31±0.03
|
| <ref name="Stella85" />
|-
|ω
| 313±10
|degree
| <ref name="Stella85" />
|-
|Τperiastron
| 2445652±1
| JD
| <ref name="Stella85" />
|-
|distance
| ~7
| kpc
| <ref name="Negueruela99" />
|}

= Description =

V 0332+53 was first recognized in Tenma observations from late 1983 to January 1984
(<ref name="Tanaka83" />, <ref name="Makishima90b" />). After the detection it was realized that it had been seen by Vela 5B in 1973
(<ref name="TerrellPriedhorsky84" />). Follow-up observations by EXOSAT discovered pulsations and allowed the determination of orbital parameters (<ref name="Stella85" />).

The Tenma observations already showed evidence for a cyclotron line at ~28 keV.
Ginga observations (2–60 keV) during an outburst in 1989 found two lines at 28.5 and 53 keV (<ref name="Makishima90" />). During the next bright outburst in 2004, INTEGRAL observations (<ref name="Pottschmidt05" />) found a third cyclotron line at ~74 keV.

= Observed pulse profiles =

[https://ui.adsabs.harvard.edu/abs/2020A%2526A...638A.152R/abstract Alonso-Hernández et al. (2022)] NuSTAR pulse profiles at different luminosities and with different pulse types. From left to right, LX ≈ 15, 8 and 1 × 1037 erg/s, the first and last have been classified as pulse type 2, the intermediate as type 0.

[[File:PP_AH2022_V0332%2B53_Fig7.png|thumb]]

[https://ui.adsabs.harvard.edu/abs/2021MNRAS.506.2156B/abstract Bykov et al. (2021)] RXTE/PCA data

[[File:PP_Bykov21_V0332%2B53.png|300px]]

[https://ui.adsabs.harvard.edu/abs/2012A%26A...540A..35S/abstract Sasaki et al. (2012)] RXTE data

[[File:PP_Sasaki2012_Fig5.png|300px]]

[https://ui.adsabs.harvard.edu/abs/2006MNRAS.371...19T/abstract Tsygankov et al. (2006)] INTEGRAL JEM-X and IBIS

[[File:PP_Tsygankov2006_Fig6.png|200px]]

[https://ui.adsabs.harvard.edu/abs/2005ApJ...630L..65Z/abstract Zhang et al. (2005)] RXTE PCA and INTEGRAL

[[File:PP_Zhang2005_Fig3.png|150px]]

= Bibliography =
'''References'''

V 0332+53

2023-09-05T14:03:05Z

Kretschmar: /* Observed pulse profiles */

[[Category:Accreting X-ray Pulsars]]

Also known as EXO 0331+530 and V BQ Cam [http://simbad.u-strasbg.fr/simbad/sim-id?Ident=V0332%2B53&NbIdent=1&Radius=2&Radius.unit=arcmin&submit=submit+id Simbad] <ref name="Tanaka83" /> <ref name="Makishima90b" />

'''Monitoring Data''':

[http://xte.mit.edu/asmlc/srcs/v0332+53.html RXTE/ASM]
[http://swift.gsfc.nasa.gov/docs/swift/results/transients/V0332p53 Swift/BAT]
[http://maxi.riken.jp/top/index.php?cid=1&jname=J0334+531 MAXI]
[http://gammaray.nsstc.nasa.gov/gbm/science/pulsars/lightcurves/v0332.html Fermi/GBM pulsed flux]
[http://integral.esac.esa.int/flashes-plots/EXO%200331+530_plot.html Current data in FLASHES]

= System Overview =

{| class="wikitable"
|Porb
| 34.25
| days
| <ref name="Stella85" />
|-
|Pspin
| ~4.4
| s
| <ref name="Stella85" />
|-
|B
| 2.7 x 1012
| G
| <ref name="Pottschmidt05" />
|-
|a sin i
| 48±4
| lt-sec
| <ref name="Stella85" />
|-
|eccentricity
| 0.31±0.03
|
| <ref name="Stella85" />
|-
|ω
| 313±10
|degree
| <ref name="Stella85" />
|-
|Τperiastron
| 2445652±1
| JD
| <ref name="Stella85" />
|-
|distance
| ~7
| kpc
| <ref name="Negueruela99" />
|}

= Description =

V 0332+53 was first recognized in Tenma observations from late 1983 to January 1984
(<ref name="Tanaka83" />, <ref name="Makishima90b" />). After the detection it was realized that it had been seen by Vela 5B in 1973
(<ref name="TerrellPriedhorsky84" />). Follow-up observations by EXOSAT discovered pulsations and allowed the determination of orbital parameters (<ref name="Stella85" />).

The Tenma observations already showed evidence for a cyclotron line at ~28 keV.
Ginga observations (2–60 keV) during an outburst in 1989 found two lines at 28.5 and 53 keV (<ref name="Makishima90" />). During the next bright outburst in 2004, INTEGRAL observations (<ref name="Pottschmidt05" />) found a third cyclotron line at ~74 keV.

= Observed pulse profiles =

[https://ui.adsabs.harvard.edu/abs/2020A%2526A...638A.152R/abstract Alonso-Hernández et al. (2022)] NuSTAR pulse profiles at different luminosities and with different pulse types. From left to right, LX ≈ 15, 8 and 1 × 1037 erg/s, the first and last have been classified as pulse type 2, the intermediate as type 0.

[[File:PP_AH2022_V0332%2B53_Fig7.png|300px]]

[https://ui.adsabs.harvard.edu/abs/2021MNRAS.506.2156B/abstract Bykov et al. (2021)] RXTE/PCA data

[[File:PP_Bykov21_V0332%2B53.png|300px]]

[https://ui.adsabs.harvard.edu/abs/2012A%26A...540A..35S/abstract Sasaki et al. (2012)] RXTE data

[[File:PP_Sasaki2012_Fig5.png|300px]]

[https://ui.adsabs.harvard.edu/abs/2006MNRAS.371...19T/abstract Tsygankov et al. (2006)] INTEGRAL JEM-X and IBIS

[[File:PP_Tsygankov2006_Fig6.png|200px]]

[https://ui.adsabs.harvard.edu/abs/2005ApJ...630L..65Z/abstract Zhang et al. (2005)] RXTE PCA and INTEGRAL

[[File:PP_Zhang2005_Fig3.png|150px]]

= Bibliography =
'''References'''

V 0332+53

2023-09-05T14:01:16Z

Kretschmar: /* Observed pulse profiles */

[[Category:Accreting X-ray Pulsars]]

Also known as EXO 0331+530 and V BQ Cam [http://simbad.u-strasbg.fr/simbad/sim-id?Ident=V0332%2B53&NbIdent=1&Radius=2&Radius.unit=arcmin&submit=submit+id Simbad] <ref name="Tanaka83" /> <ref name="Makishima90b" />

'''Monitoring Data''':

[http://xte.mit.edu/asmlc/srcs/v0332+53.html RXTE/ASM]
[http://swift.gsfc.nasa.gov/docs/swift/results/transients/V0332p53 Swift/BAT]
[http://maxi.riken.jp/top/index.php?cid=1&jname=J0334+531 MAXI]
[http://gammaray.nsstc.nasa.gov/gbm/science/pulsars/lightcurves/v0332.html Fermi/GBM pulsed flux]
[http://integral.esac.esa.int/flashes-plots/EXO%200331+530_plot.html Current data in FLASHES]

= System Overview =

{| class="wikitable"
|Porb
| 34.25
| days
| <ref name="Stella85" />
|-
|Pspin
| ~4.4
| s
| <ref name="Stella85" />
|-
|B
| 2.7 x 1012
| G
| <ref name="Pottschmidt05" />
|-
|a sin i
| 48±4
| lt-sec
| <ref name="Stella85" />
|-
|eccentricity
| 0.31±0.03
|
| <ref name="Stella85" />
|-
|ω
| 313±10
|degree
| <ref name="Stella85" />
|-
|Τperiastron
| 2445652±1
| JD
| <ref name="Stella85" />
|-
|distance
| ~7
| kpc
| <ref name="Negueruela99" />
|}

= Description =

V 0332+53 was first recognized in Tenma observations from late 1983 to January 1984
(<ref name="Tanaka83" />, <ref name="Makishima90b" />). After the detection it was realized that it had been seen by Vela 5B in 1973
(<ref name="TerrellPriedhorsky84" />). Follow-up observations by EXOSAT discovered pulsations and allowed the determination of orbital parameters (<ref name="Stella85" />).

The Tenma observations already showed evidence for a cyclotron line at ~28 keV.
Ginga observations (2–60 keV) during an outburst in 1989 found two lines at 28.5 and 53 keV (<ref name="Makishima90" />). During the next bright outburst in 2004, INTEGRAL observations (<ref name="Pottschmidt05" />) found a third cyclotron line at ~74 keV.

= Observed pulse profiles =

[https://ui.adsabs.harvard.edu/abs/2020A%2526A...638A.152R/abstract Alonso-Hernández et al. (2022)] NuSTAR pulse profiles at different luminosities and with different pulse types. From left to right, LX ≈ 15, 8 and 1 × 1037 erg/s, the first and last have been classified as pulse type 2, the intermediate as type 0.

[[File:PP_AH2022_V0332%2B53_Fig7.png|600px]]

[https://ui.adsabs.harvard.edu/abs/2021MNRAS.506.2156B/abstract Bykov et al. (2021)] RXTE/PCA data

[[File:PP_Bykov21_V0332%2B53.png|600px]]

[https://ui.adsabs.harvard.edu/abs/2012A%26A...540A..35S/abstract Sasaki et al. (2012)] RXTE data

[[File:PP_Sasaki2012_Fig5.png|600px]]

[https://ui.adsabs.harvard.edu/abs/2006MNRAS.371...19T/abstract Tsygankov et al. (2006)] INTEGRAL JEM-X and IBIS

[[File:PP_Tsygankov2006_Fig6.png|400px]]

[https://ui.adsabs.harvard.edu/abs/2005ApJ...630L..65Z/abstract Zhang et al. (2005)] RXTE PCA and INTEGRAL

[[File:PP_Zhang2005_Fig3.png|300px]]

= Bibliography =
'''References'''

V 0332+53

2023-09-05T14:00:50Z

Kretschmar: /* Observed pulse profiles */

[[Category:Accreting X-ray Pulsars]]

Also known as EXO 0331+530 and V BQ Cam [http://simbad.u-strasbg.fr/simbad/sim-id?Ident=V0332%2B53&NbIdent=1&Radius=2&Radius.unit=arcmin&submit=submit+id Simbad] <ref name="Tanaka83" /> <ref name="Makishima90b" />

'''Monitoring Data''':

[http://xte.mit.edu/asmlc/srcs/v0332+53.html RXTE/ASM]
[http://swift.gsfc.nasa.gov/docs/swift/results/transients/V0332p53 Swift/BAT]
[http://maxi.riken.jp/top/index.php?cid=1&jname=J0334+531 MAXI]
[http://gammaray.nsstc.nasa.gov/gbm/science/pulsars/lightcurves/v0332.html Fermi/GBM pulsed flux]
[http://integral.esac.esa.int/flashes-plots/EXO%200331+530_plot.html Current data in FLASHES]

= System Overview =

{| class="wikitable"
|Porb
| 34.25
| days
| <ref name="Stella85" />
|-
|Pspin
| ~4.4
| s
| <ref name="Stella85" />
|-
|B
| 2.7 x 1012
| G
| <ref name="Pottschmidt05" />
|-
|a sin i
| 48±4
| lt-sec
| <ref name="Stella85" />
|-
|eccentricity
| 0.31±0.03
|
| <ref name="Stella85" />
|-
|ω
| 313±10
|degree
| <ref name="Stella85" />
|-
|Τperiastron
| 2445652±1
| JD
| <ref name="Stella85" />
|-
|distance
| ~7
| kpc
| <ref name="Negueruela99" />
|}

= Description =

V 0332+53 was first recognized in Tenma observations from late 1983 to January 1984
(<ref name="Tanaka83" />, <ref name="Makishima90b" />). After the detection it was realized that it had been seen by Vela 5B in 1973
(<ref name="TerrellPriedhorsky84" />). Follow-up observations by EXOSAT discovered pulsations and allowed the determination of orbital parameters (<ref name="Stella85" />).

The Tenma observations already showed evidence for a cyclotron line at ~28 keV.
Ginga observations (2–60 keV) during an outburst in 1989 found two lines at 28.5 and 53 keV (<ref name="Makishima90" />). During the next bright outburst in 2004, INTEGRAL observations (<ref name="Pottschmidt05" />) found a third cyclotron line at ~74 keV.

= Observed pulse profiles =

[https://ui.adsabs.harvard.edu/abs/2020A%2526A...638A.152R/abstract Alonso-Hernández et al. (2022)] NuSTAR pulse profiles at different luminosities and with different pulse types. From left to right, LX ≈ 15, 8 and 1 × 1037 erg/s, the first and last have been classified as pulse type 2, the intermediate as type 0.

[[File:PP_AH2022_V0332%2B53_Fig7.png|600px]]

[https://ui.adsabs.harvard.edu/abs/2021MNRAS.506.2156B/abstract Bykov et al. (2021)] RXTE/PCA data

[[File:PP_Bykov21_V0332%2B53.png|600px]]

[https://ui.adsabs.harvard.edu/abs/2012A%26A...540A..35S/abstract Sasaki et al. (2012)] RXTE data

[[File:PP_Sasaki2012_Fig5.png|600px]]

[https://ui.adsabs.harvard.edu/abs/2006MNRAS.371...19T/abstract Tsygankov et al. (2006)] INTEGRAL JEM-X and IBIS

[[File:PP_Tsygankov2006_Fig6.png]]

[https://ui.adsabs.harvard.edu/abs/2005ApJ...630L..65Z/abstract Zhang et al. (2005)] RXTE PCA and INTEGRAL

[[File:PP_Zhang2005_Fig3.png|300px]]

= Bibliography =
'''References'''

File:PP Tsygankov2006 Fig6.png

2023-09-05T13:58:49Z

Kretschmar: V0332+53 pulse profiles obtained with JEM-X and IBIS for different source intensities.

== Summary ==
V0332+53 pulse profiles obtained with JEM-X and IBIS for different source intensities.

V 0332+53

2023-09-05T13:53:17Z

Kretschmar: /* Observed pulse profiles */

[[Category:Accreting X-ray Pulsars]]

Also known as EXO 0331+530 and V BQ Cam [http://simbad.u-strasbg.fr/simbad/sim-id?Ident=V0332%2B53&NbIdent=1&Radius=2&Radius.unit=arcmin&submit=submit+id Simbad] <ref name="Tanaka83" /> <ref name="Makishima90b" />

'''Monitoring Data''':

[http://xte.mit.edu/asmlc/srcs/v0332+53.html RXTE/ASM]
[http://swift.gsfc.nasa.gov/docs/swift/results/transients/V0332p53 Swift/BAT]
[http://maxi.riken.jp/top/index.php?cid=1&jname=J0334+531 MAXI]
[http://gammaray.nsstc.nasa.gov/gbm/science/pulsars/lightcurves/v0332.html Fermi/GBM pulsed flux]
[http://integral.esac.esa.int/flashes-plots/EXO%200331+530_plot.html Current data in FLASHES]

= System Overview =

{| class="wikitable"
|Porb
| 34.25
| days
| <ref name="Stella85" />
|-
|Pspin
| ~4.4
| s
| <ref name="Stella85" />
|-
|B
| 2.7 x 1012
| G
| <ref name="Pottschmidt05" />
|-
|a sin i
| 48±4
| lt-sec
| <ref name="Stella85" />
|-
|eccentricity
| 0.31±0.03
|
| <ref name="Stella85" />
|-
|ω
| 313±10
|degree
| <ref name="Stella85" />
|-
|Τperiastron
| 2445652±1
| JD
| <ref name="Stella85" />
|-
|distance
| ~7
| kpc
| <ref name="Negueruela99" />
|}

= Description =

V 0332+53 was first recognized in Tenma observations from late 1983 to January 1984
(<ref name="Tanaka83" />, <ref name="Makishima90b" />). After the detection it was realized that it had been seen by Vela 5B in 1973
(<ref name="TerrellPriedhorsky84" />). Follow-up observations by EXOSAT discovered pulsations and allowed the determination of orbital parameters (<ref name="Stella85" />).

The Tenma observations already showed evidence for a cyclotron line at ~28 keV.
Ginga observations (2–60 keV) during an outburst in 1989 found two lines at 28.5 and 53 keV (<ref name="Makishima90" />). During the next bright outburst in 2004, INTEGRAL observations (<ref name="Pottschmidt05" />) found a third cyclotron line at ~74 keV.

= Observed pulse profiles =

[https://ui.adsabs.harvard.edu/abs/2020A%2526A...638A.152R/abstract Alonso-Hernández et al. (2022)] NuSTAR pulse profiles at different luminosities and with different pulse types. From left to right, LX ≈ 15, 8 and 1 × 1037 erg/s, the first and last have been classified as pulse type 2, the intermediate as type 0.

[[File:PP_AH2022_V0332%2B53_Fig7.png|600px]]

[https://ui.adsabs.harvard.edu/abs/2021MNRAS.506.2156B/abstract Bykov et al. (2021)] RXTE/PCA data

[[File:PP_Bykov21_V0332%2B53.png|600px]]

[https://ui.adsabs.harvard.edu/abs/2012A%26A...540A..35S/abstract Sasaki et al. (2012)] RXTE data

[[File:PP_Sasaki2012_Fig5.png|600px]]

[https://ui.adsabs.harvard.edu/abs/2005ApJ...630L..65Z/abstract Zhang et al. (2005)] RXTE PCA and INTEGRAL

[[File:PP_Zhang2005_Fig3.png|300px]]

= Bibliography =
'''References'''

V 0332+53

2023-09-05T13:52:41Z

Kretschmar: /* Observed pulse profiles */

[[Category:Accreting X-ray Pulsars]]

Also known as EXO 0331+530 and V BQ Cam [http://simbad.u-strasbg.fr/simbad/sim-id?Ident=V0332%2B53&NbIdent=1&Radius=2&Radius.unit=arcmin&submit=submit+id Simbad] <ref name="Tanaka83" /> <ref name="Makishima90b" />

'''Monitoring Data''':

[http://xte.mit.edu/asmlc/srcs/v0332+53.html RXTE/ASM]
[http://swift.gsfc.nasa.gov/docs/swift/results/transients/V0332p53 Swift/BAT]
[http://maxi.riken.jp/top/index.php?cid=1&jname=J0334+531 MAXI]
[http://gammaray.nsstc.nasa.gov/gbm/science/pulsars/lightcurves/v0332.html Fermi/GBM pulsed flux]
[http://integral.esac.esa.int/flashes-plots/EXO%200331+530_plot.html Current data in FLASHES]

= System Overview =

{| class="wikitable"
|Porb
| 34.25
| days
| <ref name="Stella85" />
|-
|Pspin
| ~4.4
| s
| <ref name="Stella85" />
|-
|B
| 2.7 x 1012
| G
| <ref name="Pottschmidt05" />
|-
|a sin i
| 48±4
| lt-sec
| <ref name="Stella85" />
|-
|eccentricity
| 0.31±0.03
|
| <ref name="Stella85" />
|-
|ω
| 313±10
|degree
| <ref name="Stella85" />
|-
|Τperiastron
| 2445652±1
| JD
| <ref name="Stella85" />
|-
|distance
| ~7
| kpc
| <ref name="Negueruela99" />
|}

= Description =

V 0332+53 was first recognized in Tenma observations from late 1983 to January 1984
(<ref name="Tanaka83" />, <ref name="Makishima90b" />). After the detection it was realized that it had been seen by Vela 5B in 1973
(<ref name="TerrellPriedhorsky84" />). Follow-up observations by EXOSAT discovered pulsations and allowed the determination of orbital parameters (<ref name="Stella85" />).

The Tenma observations already showed evidence for a cyclotron line at ~28 keV.
Ginga observations (2–60 keV) during an outburst in 1989 found two lines at 28.5 and 53 keV (<ref name="Makishima90" />). During the next bright outburst in 2004, INTEGRAL observations (<ref name="Pottschmidt05" />) found a third cyclotron line at ~74 keV.

= Observed pulse profiles =

[https://ui.adsabs.harvard.edu/abs/2020A%2526A...638A.152R/abstract Alonso-Hernández et al. (2022)] NuSTAR pulse profiles at different luminosities and with different pulse types. From left to right, LX ≈ 15, 8 and 1 × 1037 erg/s, the first and last have been classified as pulse type 2, the intermediate as type 0.

[[File:PP_AH2022_V0332%2B53_Fig7.png|600px]]

[https://ui.adsabs.harvard.edu/abs/2021MNRAS.506.2156B/abstract Bykov et al. (2021)] RXTE/PCA data

[[File:PP_Bykov21_V0332%2B53.png|600px]]

[https://ui.adsabs.harvard.edu/abs/2012A%26A...540A..35S/abstract Sasaki et al. (2012)] RXTE data

[[File:PP_Sasaki2012_Fig5.png|600px]]

[https://ui.adsabs.harvard.edu/abs/2005ApJ...630L..65Z/abstract Zhang et al. (2005)] RXTE PCA and INTEGRAL

[[File:PP_Zhang2005_Fig3.png|600px]]

= Bibliography =
'''References'''

File:AH2022 V0332+53 Fig7.png

2023-09-05T13:52:19Z

Kretschmar: Kretschmar moved page File:AH2022 V0332+53 Fig7.png to File:PP AH2022 V0332+53 Fig7.png

#REDIRECT [[File:PP AH2022 V0332+53 Fig7.png]]

File:PP AH2022 V0332+53 Fig7.png

2023-09-05T13:52:19Z

Kretschmar: Kretschmar moved page File:AH2022 V0332+53 Fig7.png to File:PP AH2022 V0332+53 Fig7.png

== Summary ==
Comparison of normalized pulse profiles of source V 0332+53 studied at different energy ranges in different stages during a flare period.

File:Bykov21 V0332+53.png

2023-09-05T13:51:46Z

Kretschmar: Kretschmar moved page File:Bykov21 V0332+53.png to File:PP Bykov21 V0332+53.png

#REDIRECT [[File:PP Bykov21 V0332+53.png]]

File:PP Bykov21 V0332+53.png

2023-09-05T13:51:46Z

Kretschmar: Kretschmar moved page File:Bykov21 V0332+53.png to File:PP Bykov21 V0332+53.png

== Summary ==
3–12 keV pulse profiles

V 0332+53

2023-09-05T13:48:31Z

Kretschmar: /* Observed pulse profiles */

[[Category:Accreting X-ray Pulsars]]

Also known as EXO 0331+530 and V BQ Cam [http://simbad.u-strasbg.fr/simbad/sim-id?Ident=V0332%2B53&NbIdent=1&Radius=2&Radius.unit=arcmin&submit=submit+id Simbad] <ref name="Tanaka83" /> <ref name="Makishima90b" />

'''Monitoring Data''':

[http://xte.mit.edu/asmlc/srcs/v0332+53.html RXTE/ASM]
[http://swift.gsfc.nasa.gov/docs/swift/results/transients/V0332p53 Swift/BAT]
[http://maxi.riken.jp/top/index.php?cid=1&jname=J0334+531 MAXI]
[http://gammaray.nsstc.nasa.gov/gbm/science/pulsars/lightcurves/v0332.html Fermi/GBM pulsed flux]
[http://integral.esac.esa.int/flashes-plots/EXO%200331+530_plot.html Current data in FLASHES]

= System Overview =

{| class="wikitable"
|Porb
| 34.25
| days
| <ref name="Stella85" />
|-
|Pspin
| ~4.4
| s
| <ref name="Stella85" />
|-
|B
| 2.7 x 1012
| G
| <ref name="Pottschmidt05" />
|-
|a sin i
| 48±4
| lt-sec
| <ref name="Stella85" />
|-
|eccentricity
| 0.31±0.03
|
| <ref name="Stella85" />
|-
|ω
| 313±10
|degree
| <ref name="Stella85" />
|-
|Τperiastron
| 2445652±1
| JD
| <ref name="Stella85" />
|-
|distance
| ~7
| kpc
| <ref name="Negueruela99" />
|}

= Description =

V 0332+53 was first recognized in Tenma observations from late 1983 to January 1984
(<ref name="Tanaka83" />, <ref name="Makishima90b" />). After the detection it was realized that it had been seen by Vela 5B in 1973
(<ref name="TerrellPriedhorsky84" />). Follow-up observations by EXOSAT discovered pulsations and allowed the determination of orbital parameters (<ref name="Stella85" />).

The Tenma observations already showed evidence for a cyclotron line at ~28 keV.
Ginga observations (2–60 keV) during an outburst in 1989 found two lines at 28.5 and 53 keV (<ref name="Makishima90" />). During the next bright outburst in 2004, INTEGRAL observations (<ref name="Pottschmidt05" />) found a third cyclotron line at ~74 keV.

= Observed pulse profiles =

[https://ui.adsabs.harvard.edu/abs/2020A%2526A...638A.152R/abstract Alonso-Hernández et al. (2022)] NuSTAR pulse profiles at different luminosities and with different pulse types. From left to right, LX ≈ 15, 8 and 1 × 1037 erg/s, the first and last have been classified as pulse type 2, the intermediate as type 0.

[[File:AH2022_V0332%2B53_Fig7.png|600px]]

[https://ui.adsabs.harvard.edu/abs/2021MNRAS.506.2156B/abstract Bykov et al. (2021)] RXTE/PCA data

[[File:Bykov21_V0332%2B53.png|600px]]

[https://ui.adsabs.harvard.edu/abs/2012A%26A...540A..35S/abstract Sasaki et al. (2012)] RXTE data

[[File:PP_Sasaki2012_Fig5.png|600px]]

[https://ui.adsabs.harvard.edu/abs/2005ApJ...630L..65Z/abstract Zhang et al. (2005)] RXTE PCA and INTEGRAL

[[File:PP_Zhang2005_Fig3.png|600px]]

= Bibliography =
'''References'''

File:Sasaki2012 Fig5.png

2023-09-05T13:47:28Z

Kretschmar: Kretschmar moved page File:Sasaki2012 Fig5.png to File:PP Sasaki2012 Fig5.png

#REDIRECT [[File:PP Sasaki2012 Fig5.png]]

File:PP Sasaki2012 Fig5.png

2023-09-05T13:47:28Z

Kretschmar: Kretschmar moved page File:Sasaki2012 Fig5.png to File:PP Sasaki2012 Fig5.png

== Summary ==
Pulse profiles of V 0332+53 during the giant outburst in 2004/2005 observed with RXTE

V 0332+53

2023-09-05T13:43:19Z

Kretschmar: /* Observed pulse profiles */

[[Category:Accreting X-ray Pulsars]]

Also known as EXO 0331+530 and V BQ Cam [http://simbad.u-strasbg.fr/simbad/sim-id?Ident=V0332%2B53&NbIdent=1&Radius=2&Radius.unit=arcmin&submit=submit+id Simbad] <ref name="Tanaka83" /> <ref name="Makishima90b" />

'''Monitoring Data''':

[http://xte.mit.edu/asmlc/srcs/v0332+53.html RXTE/ASM]
[http://swift.gsfc.nasa.gov/docs/swift/results/transients/V0332p53 Swift/BAT]
[http://maxi.riken.jp/top/index.php?cid=1&jname=J0334+531 MAXI]
[http://gammaray.nsstc.nasa.gov/gbm/science/pulsars/lightcurves/v0332.html Fermi/GBM pulsed flux]
[http://integral.esac.esa.int/flashes-plots/EXO%200331+530_plot.html Current data in FLASHES]

= System Overview =

{| class="wikitable"
|Porb
| 34.25
| days
| <ref name="Stella85" />
|-
|Pspin
| ~4.4
| s
| <ref name="Stella85" />
|-
|B
| 2.7 x 1012
| G
| <ref name="Pottschmidt05" />
|-
|a sin i
| 48±4
| lt-sec
| <ref name="Stella85" />
|-
|eccentricity
| 0.31±0.03
|
| <ref name="Stella85" />
|-
|ω
| 313±10
|degree
| <ref name="Stella85" />
|-
|Τperiastron
| 2445652±1
| JD
| <ref name="Stella85" />
|-
|distance
| ~7
| kpc
| <ref name="Negueruela99" />
|}

= Description =

V 0332+53 was first recognized in Tenma observations from late 1983 to January 1984
(<ref name="Tanaka83" />, <ref name="Makishima90b" />). After the detection it was realized that it had been seen by Vela 5B in 1973
(<ref name="TerrellPriedhorsky84" />). Follow-up observations by EXOSAT discovered pulsations and allowed the determination of orbital parameters (<ref name="Stella85" />).

The Tenma observations already showed evidence for a cyclotron line at ~28 keV.
Ginga observations (2–60 keV) during an outburst in 1989 found two lines at 28.5 and 53 keV (<ref name="Makishima90" />). During the next bright outburst in 2004, INTEGRAL observations (<ref name="Pottschmidt05" />) found a third cyclotron line at ~74 keV.

= Observed pulse profiles =

[https://ui.adsabs.harvard.edu/abs/2020A%2526A...638A.152R/abstract Alonso-Hernández et al. (2022)] NuSTAR pulse profiles at different luminosities and with different pulse types. From left to right, LX ≈ 15, 8 and 1 × 1037 erg/s, the first and last have been classified as pulse type 2, the intermediate as type 0.

[[File:AH2022_V0332%2B53_Fig7.png|600px]]

[https://ui.adsabs.harvard.edu/abs/2021MNRAS.506.2156B/abstract Bykov et al. (2021)] RXTE/PCA data

[[File:Bykov21_V0332%2B53.png|600px]]

[https://ui.adsabs.harvard.edu/abs/2012A%26A...540A..35S/abstract Sasaki et al. (2012)] RXTE data

[[File:Sasaki2012_Fig5.png|600px]]

[https://ui.adsabs.harvard.edu/abs/2005ApJ...630L..65Z/abstract Zhang et al. (2005)] RXTE PCA and INTEGRAL

[[File:PP_Zhang2005_Fig3.png]]

= Bibliography =
'''References'''

File:PP Zhang2005 Fig3.png

2023-09-05T13:42:39Z

Kretschmar: Pulse profiles at different intensity states of V0332+53

== Summary ==
Pulse profiles at different intensity states of V0332+53

V 0332+53

2023-09-05T13:30:37Z

Kretschmar:

[[Category:Accreting X-ray Pulsars]]

Also known as EXO 0331+530 and V BQ Cam [http://simbad.u-strasbg.fr/simbad/sim-id?Ident=V0332%2B53&NbIdent=1&Radius=2&Radius.unit=arcmin&submit=submit+id Simbad] <ref name="Tanaka83" /> <ref name="Makishima90b" />

'''Monitoring Data''':

[http://xte.mit.edu/asmlc/srcs/v0332+53.html RXTE/ASM]
[http://swift.gsfc.nasa.gov/docs/swift/results/transients/V0332p53 Swift/BAT]
[http://maxi.riken.jp/top/index.php?cid=1&jname=J0334+531 MAXI]
[http://gammaray.nsstc.nasa.gov/gbm/science/pulsars/lightcurves/v0332.html Fermi/GBM pulsed flux]
[http://integral.esac.esa.int/flashes-plots/EXO%200331+530_plot.html Current data in FLASHES]

= System Overview =

{| class="wikitable"
|Porb
| 34.25
| days
| <ref name="Stella85" />
|-
|Pspin
| ~4.4
| s
| <ref name="Stella85" />
|-
|B
| 2.7 x 1012
| G
| <ref name="Pottschmidt05" />
|-
|a sin i
| 48±4
| lt-sec
| <ref name="Stella85" />
|-
|eccentricity
| 0.31±0.03
|
| <ref name="Stella85" />
|-
|ω
| 313±10
|degree
| <ref name="Stella85" />
|-
|Τperiastron
| 2445652±1
| JD
| <ref name="Stella85" />
|-
|distance
| ~7
| kpc
| <ref name="Negueruela99" />
|}

= Description =

V 0332+53 was first recognized in Tenma observations from late 1983 to January 1984
(<ref name="Tanaka83" />, <ref name="Makishima90b" />). After the detection it was realized that it had been seen by Vela 5B in 1973
(<ref name="TerrellPriedhorsky84" />). Follow-up observations by EXOSAT discovered pulsations and allowed the determination of orbital parameters (<ref name="Stella85" />).

The Tenma observations already showed evidence for a cyclotron line at ~28 keV.
Ginga observations (2–60 keV) during an outburst in 1989 found two lines at 28.5 and 53 keV (<ref name="Makishima90" />). During the next bright outburst in 2004, INTEGRAL observations (<ref name="Pottschmidt05" />) found a third cyclotron line at ~74 keV.

= Observed pulse profiles =

[https://ui.adsabs.harvard.edu/abs/2020A%2526A...638A.152R/abstract Alonso-Hernández et al. (2022)] NuSTAR pulse profiles at different luminosities and with different pulse types. From left to right, LX ≈ 15, 8 and 1 × 1037 erg/s, the first and last have been classified as pulse type 2, the intermediate as type 0.

[[File:AH2022_V0332%2B53_Fig7.png|600px]]

[https://ui.adsabs.harvard.edu/abs/2021MNRAS.506.2156B/abstract Bykov et al. (2021)] RXTE/PCA data

[[File:Bykov21_V0332%2B53.png|600px]]

[https://ui.adsabs.harvard.edu/abs/2012A%26A...540A..35S/abstract Sasaki et al. (2012)] RXTE data

[[File:Sasaki2012_Fig5.png|600px]]

= Bibliography =
'''References'''

V 0332+53

2023-09-05T13:29:52Z

Kretschmar: /* Observed pulse profiles */

[[Category:Accreting X-ray Pulsars]]

Also known as EXO 0331+530 and V BQ Cam [http://simbad.u-strasbg.fr/simbad/sim-id?Ident=V0332%2B53&NbIdent=1&Radius=2&Radius.unit=arcmin&submit=submit+id Simbad] <ref name="Tanaka83" /> <ref name="Makishima90b" />

'''Monitoring Data''':

[http://xte.mit.edu/asmlc/srcs/v0332+53.html RXTE/ASM]
[http://swift.gsfc.nasa.gov/docs/swift/results/transients/V0332p53 Swift/BAT]
[http://maxi.riken.jp/top/index.php?cid=1&jname=J0334+531 MAXI]
[http://gammaray.nsstc.nasa.gov/gbm/science/pulsars/lightcurves/v0332.html Fermi/GBM pulsed flux]
[http://integral.esac.esa.int/flashes-plots/EXO%200331+530_plot.html Current data in FLASHES]

= System Overview =

{| class="wikitable"
|Porb
| 34.25
| days
| <ref name="Stella85" />
|-
|Pspin
| ~4.4
| s
| <ref name="Stella85" />
|-
|B
| 2.7 x 1012
| G
| <ref name="Pottschmidt05" />
|-
|a sin i
| 48±4
| lt-sec
| <ref name="Stella85" />
|-
|eccentricity
| 0.31±0.03
|
| <ref name="Stella85" />
|-
|ω
| 313±10
|degree
| <ref name="Stella85" />
|-
|Τperiastron
| 2445652±1
| JD
| <ref name="Stella85" />
|-
|distance
| ~7
| kpc
| <ref name="Negueruela99" />
|}

= Description =

V 0332+53 was first recognized in Tenma observations from late 1983 to January 1984
(<ref name="Tanaka83" />, <ref name="Makishima90b" />). After the detection it was realized that it had been seen by Vela 5B in 1973
(<ref name="TerrellPriedhorsky84" />). Follow-up observations by EXOSAT discovered pulsations and allowed the determination of orbital parameters (<ref name="Stella85" />).

The Tenma observations already showed evidence for a cyclotron line at ~28 keV.
Ginga observations (2–60 keV) during an outburst in 1989 found two lines at 28.5 and 53 keV (<ref name="Makishima90" />). During the next bright outburst in 2004, INTEGRAL observations (<ref name="Pottschmidt05" />) found a third cyclotron line at ~74 keV.

= Observed pulse profiles =

[https://ui.adsabs.harvard.edu/abs/2020A%2526A...638A.152R/abstract Alonso-Hernández et al. (2022)] NuSTAR pulse profiles at different luminosities and with different pulse types. From left to right, LX ≈ 15, 8 and 1 × 1037 erg/s, the first and last have been classified as pulse type 2, the intermediate as type 0.

[[File:AH2022_V0332%2B53_Fig7.png|600px]]

[https://ui.adsabs.harvard.edu/abs/2021MNRAS.506.2156B/abstract Bykov et al. (2021)] RXTE/PCA data

[[File:Bykov21_V0332%2B53.png|600px]]

[https://ui.adsabs.harvard.edu/abs/2012A%26A...540A..35S/abstract Sasaki et al. (2012)] RXTE data
[[File:Sasaki2012_Fig5.png|600px]]

'''References'''

File:PP Sasaki2012 Fig5.png

2023-09-05T13:28:47Z

Kretschmar: Pulse profiles of V 0332+53 during the giant outburst in 2004/2005 observed with RXTE

== Summary ==
Pulse profiles of V 0332+53 during the giant outburst in 2004/2005 observed with RXTE

V 0332+53

2023-09-05T13:22:23Z

Kretschmar: /* Observed pulse profiles */

[[Category:Accreting X-ray Pulsars]]

Also known as EXO 0331+530 and V BQ Cam [http://simbad.u-strasbg.fr/simbad/sim-id?Ident=V0332%2B53&NbIdent=1&Radius=2&Radius.unit=arcmin&submit=submit+id Simbad] <ref name="Tanaka83" /> <ref name="Makishima90b" />

'''Monitoring Data''':

[http://xte.mit.edu/asmlc/srcs/v0332+53.html RXTE/ASM]
[http://swift.gsfc.nasa.gov/docs/swift/results/transients/V0332p53 Swift/BAT]
[http://maxi.riken.jp/top/index.php?cid=1&jname=J0334+531 MAXI]
[http://gammaray.nsstc.nasa.gov/gbm/science/pulsars/lightcurves/v0332.html Fermi/GBM pulsed flux]
[http://integral.esac.esa.int/flashes-plots/EXO%200331+530_plot.html Current data in FLASHES]

= System Overview =

{| class="wikitable"
|Porb
| 34.25
| days
| <ref name="Stella85" />
|-
|Pspin
| ~4.4
| s
| <ref name="Stella85" />
|-
|B
| 2.7 x 1012
| G
| <ref name="Pottschmidt05" />
|-
|a sin i
| 48±4
| lt-sec
| <ref name="Stella85" />
|-
|eccentricity
| 0.31±0.03
|
| <ref name="Stella85" />
|-
|ω
| 313±10
|degree
| <ref name="Stella85" />
|-
|Τperiastron
| 2445652±1
| JD
| <ref name="Stella85" />
|-
|distance
| ~7
| kpc
| <ref name="Negueruela99" />
|}

= Description =

V 0332+53 was first recognized in Tenma observations from late 1983 to January 1984
(<ref name="Tanaka83" />, <ref name="Makishima90b" />). After the detection it was realized that it had been seen by Vela 5B in 1973
(<ref name="TerrellPriedhorsky84" />). Follow-up observations by EXOSAT discovered pulsations and allowed the determination of orbital parameters (<ref name="Stella85" />).

The Tenma observations already showed evidence for a cyclotron line at ~28 keV.
Ginga observations (2–60 keV) during an outburst in 1989 found two lines at 28.5 and 53 keV (<ref name="Makishima90" />). During the next bright outburst in 2004, INTEGRAL observations (<ref name="Pottschmidt05" />) found a third cyclotron line at ~74 keV.

= Observed pulse profiles =

[https://ui.adsabs.harvard.edu/abs/2020A%2526A...638A.152R/abstract Alonso-Hernández et al. (2022)] NuSTAR pulse profiles at different luminosities and with different pulse types. From left to right, LX ≈ 15, 8 and 1 × 1037 erg/s, the first and last have been classified as pulse type 2, the intermediate as type 0.

[[File:AH2022_V0332%2B53_Fig7.png|600px]]

[https://ui.adsabs.harvard.edu/abs/2021MNRAS.506.2156B/abstract Bykov et al. (2021)] RXTE/PCA data

[[File:Bykov21_V0332%2B53.png|600px]]

[https://ui.adsabs.harvard.edu/abs/2012A%26A...540A..35S/abstract Sasaki et al. (2012)] RXTE data

'''References'''

V 0332+53

2023-09-05T13:17:18Z

Kretschmar: /* Observed pulse profiles */

[[Category:Accreting X-ray Pulsars]]

Also known as EXO 0331+530 and V BQ Cam [http://simbad.u-strasbg.fr/simbad/sim-id?Ident=V0332%2B53&NbIdent=1&Radius=2&Radius.unit=arcmin&submit=submit+id Simbad] <ref name="Tanaka83" /> <ref name="Makishima90b" />

'''Monitoring Data''':

[http://xte.mit.edu/asmlc/srcs/v0332+53.html RXTE/ASM]
[http://swift.gsfc.nasa.gov/docs/swift/results/transients/V0332p53 Swift/BAT]
[http://maxi.riken.jp/top/index.php?cid=1&jname=J0334+531 MAXI]
[http://gammaray.nsstc.nasa.gov/gbm/science/pulsars/lightcurves/v0332.html Fermi/GBM pulsed flux]
[http://integral.esac.esa.int/flashes-plots/EXO%200331+530_plot.html Current data in FLASHES]

= System Overview =

{| class="wikitable"
|Porb
| 34.25
| days
| <ref name="Stella85" />
|-
|Pspin
| ~4.4
| s
| <ref name="Stella85" />
|-
|B
| 2.7 x 1012
| G
| <ref name="Pottschmidt05" />
|-
|a sin i
| 48±4
| lt-sec
| <ref name="Stella85" />
|-
|eccentricity
| 0.31±0.03
|
| <ref name="Stella85" />
|-
|ω
| 313±10
|degree
| <ref name="Stella85" />
|-
|Τperiastron
| 2445652±1
| JD
| <ref name="Stella85" />
|-
|distance
| ~7
| kpc
| <ref name="Negueruela99" />
|}

= Description =

V 0332+53 was first recognized in Tenma observations from late 1983 to January 1984
(<ref name="Tanaka83" />, <ref name="Makishima90b" />). After the detection it was realized that it had been seen by Vela 5B in 1973
(<ref name="TerrellPriedhorsky84" />). Follow-up observations by EXOSAT discovered pulsations and allowed the determination of orbital parameters (<ref name="Stella85" />).

The Tenma observations already showed evidence for a cyclotron line at ~28 keV.
Ginga observations (2–60 keV) during an outburst in 1989 found two lines at 28.5 and 53 keV (<ref name="Makishima90" />). During the next bright outburst in 2004, INTEGRAL observations (<ref name="Pottschmidt05" />) found a third cyclotron line at ~74 keV.

= Observed pulse profiles =

[https://ui.adsabs.harvard.edu/abs/2020A%2526A...638A.152R/abstract Alonso-Hernández et al. (2022)] NuSTAR pulse profiles at different luminosities and with different pulse types. From left to right, LX ≈ 15, 8 and 1 × 1037 erg/s, the first and last have been classified as pulse type 2, the intermediate as type 0.

[[File:AH2022_V0332%2B53_Fig7.png|600px]]

[https://ui.adsabs.harvard.edu/abs/2021MNRAS.506.2156B/abstract Bykov et al. (2021)] RXTE/PCA data

[[File:Bykov21_V0332%2B53.png|600px]]

'''References'''

V 0332+53

2023-09-05T13:16:05Z

Kretschmar: /* Observed pulse profiles */

[[Category:Accreting X-ray Pulsars]]

Also known as EXO 0331+530 and V BQ Cam [http://simbad.u-strasbg.fr/simbad/sim-id?Ident=V0332%2B53&NbIdent=1&Radius=2&Radius.unit=arcmin&submit=submit+id Simbad] <ref name="Tanaka83" /> <ref name="Makishima90b" />

'''Monitoring Data''':

[http://xte.mit.edu/asmlc/srcs/v0332+53.html RXTE/ASM]
[http://swift.gsfc.nasa.gov/docs/swift/results/transients/V0332p53 Swift/BAT]
[http://maxi.riken.jp/top/index.php?cid=1&jname=J0334+531 MAXI]
[http://gammaray.nsstc.nasa.gov/gbm/science/pulsars/lightcurves/v0332.html Fermi/GBM pulsed flux]
[http://integral.esac.esa.int/flashes-plots/EXO%200331+530_plot.html Current data in FLASHES]

= System Overview =

{| class="wikitable"
|Porb
| 34.25
| days
| <ref name="Stella85" />
|-
|Pspin
| ~4.4
| s
| <ref name="Stella85" />
|-
|B
| 2.7 x 1012
| G
| <ref name="Pottschmidt05" />
|-
|a sin i
| 48±4
| lt-sec
| <ref name="Stella85" />
|-
|eccentricity
| 0.31±0.03
|
| <ref name="Stella85" />
|-
|ω
| 313±10
|degree
| <ref name="Stella85" />
|-
|Τperiastron
| 2445652±1
| JD
| <ref name="Stella85" />
|-
|distance
| ~7
| kpc
| <ref name="Negueruela99" />
|}

= Description =

V 0332+53 was first recognized in Tenma observations from late 1983 to January 1984
(<ref name="Tanaka83" />, <ref name="Makishima90b" />). After the detection it was realized that it had been seen by Vela 5B in 1973
(<ref name="TerrellPriedhorsky84" />). Follow-up observations by EXOSAT discovered pulsations and allowed the determination of orbital parameters (<ref name="Stella85" />).

The Tenma observations already showed evidence for a cyclotron line at ~28 keV.
Ginga observations (2–60 keV) during an outburst in 1989 found two lines at 28.5 and 53 keV (<ref name="Makishima90" />). During the next bright outburst in 2004, INTEGRAL observations (<ref name="Pottschmidt05" />) found a third cyclotron line at ~74 keV.

= Observed pulse profiles =

[https://ui.adsabs.harvard.edu/abs/2020A%2526A...638A.152R/abstract Alonso-Hernández et al. (2022), A&A 662, A62: NuSTAR pulse profiles at different luminosities and with different pulse types. From left to right, LX ≈ 15, 8 and 1 × 1037 erg/s, the first and last have been classified as pulse type 2, the intermediate as type 0.

[[File:AH2022_V0332%2B53_Fig7.png|500px]]

[https://ui.adsabs.harvard.edu/abs/2021MNRAS.506.2156B/abstract Bykov et al. (2021)] RXTE/PCA data

[[File:Bykov21_V0332%2B53.png|500px]]

'''References'''

V 0332+53

2023-09-05T13:14:50Z

Kretschmar: Added pulse profles

[[Category:Accreting X-ray Pulsars]]

Also known as EXO 0331+530 and V BQ Cam [http://simbad.u-strasbg.fr/simbad/sim-id?Ident=V0332%2B53&NbIdent=1&Radius=2&Radius.unit=arcmin&submit=submit+id Simbad] <ref name="Tanaka83" /> <ref name="Makishima90b" />

'''Monitoring Data''':

[http://xte.mit.edu/asmlc/srcs/v0332+53.html RXTE/ASM]
[http://swift.gsfc.nasa.gov/docs/swift/results/transients/V0332p53 Swift/BAT]
[http://maxi.riken.jp/top/index.php?cid=1&jname=J0334+531 MAXI]
[http://gammaray.nsstc.nasa.gov/gbm/science/pulsars/lightcurves/v0332.html Fermi/GBM pulsed flux]
[http://integral.esac.esa.int/flashes-plots/EXO%200331+530_plot.html Current data in FLASHES]

= System Overview =

{| class="wikitable"
|Porb
| 34.25
| days
| <ref name="Stella85" />
|-
|Pspin
| ~4.4
| s
| <ref name="Stella85" />
|-
|B
| 2.7 x 1012
| G
| <ref name="Pottschmidt05" />
|-
|a sin i
| 48±4
| lt-sec
| <ref name="Stella85" />
|-
|eccentricity
| 0.31±0.03
|
| <ref name="Stella85" />
|-
|ω
| 313±10
|degree
| <ref name="Stella85" />
|-
|Τperiastron
| 2445652±1
| JD
| <ref name="Stella85" />
|-
|distance
| ~7
| kpc
| <ref name="Negueruela99" />
|}

= Description =

V 0332+53 was first recognized in Tenma observations from late 1983 to January 1984
(<ref name="Tanaka83" />, <ref name="Makishima90b" />). After the detection it was realized that it had been seen by Vela 5B in 1973
(<ref name="TerrellPriedhorsky84" />). Follow-up observations by EXOSAT discovered pulsations and allowed the determination of orbital parameters (<ref name="Stella85" />).

The Tenma observations already showed evidence for a cyclotron line at ~28 keV.
Ginga observations (2–60 keV) during an outburst in 1989 found two lines at 28.5 and 53 keV (<ref name="Makishima90" />). During the next bright outburst in 2004, INTEGRAL observations (<ref name="Pottschmidt05" />) found a third cyclotron line at ~74 keV.

= Observed pulse profiles =

[https://ui.adsabs.harvard.edu/abs/2020A%2526A...638A.152R/abstract Alonso-Hernández et al. (2022), A&A 662, A62: NuSTAR pulse profiles at different luminosities and with different pulse types. From left to right, LX ≈ 15, 8 and 1 × 1037 erg/s, the first and last have been classified as pulse type 2, the intermediate as type 0.
[[File:AH2022_V0332%2B53_Fig7.png]]

[https://ui.adsabs.harvard.edu/abs/2021MNRAS.506.2156B/abstract Bykov et al. (2021)] RXTE/PCA data
[[File:Bykov21_V0332%2B53.png]]

'''References'''

File:PP Bykov21 V0332+53.png

2023-09-05T13:00:22Z

Kretschmar: 3–12 keV pulse profiles

== Summary ==
3–12 keV pulse profiles

File:PP AH2022 V0332+53 Fig7.png

2023-09-05T12:58:05Z

Kretschmar: Comparison of normalized pulse profiles of source V 0332+53 studied at different energy ranges in different stages during a flare period.

== Summary ==
Comparison of normalized pulse profiles of source V 0332+53 studied at different energy ranges in different stages during a flare period.

V 0332+53

2023-09-05T12:55:00Z

Kretschmar: