J/A+A/608/A36 IGR J19552+0044 BV light curves and spectra (Tovmassian+, 2017)
IGR J19552+0044: a new asynchronous short period polar.
Filling the gap between intermediate and ordinary polars.
Tovmassian G.H., Gonzalez-Buitrago D., Thorstensen J., Kotze E.,
Breytenbach H., Schwope A., Bernardini F., Zharikov S.V., Hernandez M.S.,
Buckley D.A.H., de Miguel E., Hambsch F.-J., Myers G., Goff W., Cejudo D.,
Starkey D., Campbell T., Ulowetz J., Stein W., Nelson P., Reichart D.E.,
Haislip J.B., Ivarsen K.M., LaCluyze A.P., Moore J.P., Miroshnichenko A.S.
<Astron. Astrophys. 608, A36 (2017)>
=2017A&A...608A..36T 2017A&A...608A..36T (SIMBAD/NED BibCode)
ADC_Keywords: Binaries, cataclysmic ; Photometry ; Spectroscopy
Keywords: binaries: close - novae, cataclysmic variables - magnetic field
Abstract:
Based on XMM-Newton X-ray observations IGR J19552+0044 appears to be
either a pre-polar or an asynchronous polar. Aims. We conducted
follow-up optical observations to identify the sources and periods of
variability precisely and to classify this X-ray source correctly.
Extensive multicolor photometric and medium- to high-resolution
spectroscopy observations were performed and period search codes were
applied to sort out the complex variability of the object.
We found firm evidence of discording spectroscopic (81.29±0.01m)
and photometric (83.599±0.002m) periods that we ascribe to the
white dwarf (WD) spin period and binary orbital period, respectively.
This confirms that IGR J19552+0044 is an asynchronous polar.
Wavelength dependent variability and its continuously changing shape
point at a cyclotron emission from a magnetic WD with a relatively low
magnetic field below 20MG.
The difference between the WD spin period and the binary orbital
period proves that IGR J19552+0044 is a polar with the largest known
degree of asynchronism (0.97 or 3%).
Description:
The files contain photometric data in V and I filters as well as
spectra of the object obtained in low resolution mode. The data are
reduced to magnitudes at heliocentric times indicating mid-exposure.
The magnitudes in Johnson V- and I-bands are calibrated using the
secondary standards in the filed of the object. The spectra are flux
and wavelength calibrated. Some spectra suffer from inadequate
subtraction of telluric lines.
Objects:
---------------------------------------------------------------------
RA (2000) DE Designation(s)
---------------------------------------------------------------------
19 55 12.47 +00 45 36.6 IGR J19552+0044 = 2MASS J19551247+0045365
---------------------------------------------------------------------
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
list.dat 79 41 List of spectra
sp/* . 41 Individual fits spectra
iband.dat 24 4658 I band photometry of IGR J19552+0044
vband.dat 24 2578 V band photometry of IGR J19552+0044
--------------------------------------------------------------------------------
Byte-by-byte Description of file: list.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 25 A25 --- FileName Name of the spectrum file in subdirectory sp
27- 36 A10 "date" Obs.Date Observation date
38- 40 I3 --- Nsp Spectrum number within the observation date
42- 79 A38 --- Title Title of the file
--------------------------------------------------------------------------------
Byte-by-byte Description of file: iband.dat vband.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 11 F11.6 --- HJD Heliocentric Julian date (HJD-2450000)
13- 17 F5.2 mag mag Magnitude in Band
19- 22 F4.2 mag e_mag rms uncertainty on mag
24 A1 --- Band [IV] Observed band (Johnson)
--------------------------------------------------------------------------------
Acknowledgements:
Gagik Tovmassian, gag(at)astro.unam.mx
(End) Gagik Tovmassian[OAN SAT, Mexico], Patricia Vannier [CDS] 05-Dec-2017