J/A+A/659/L2 5 QPE X-ray sources spectra (Wevers+, 2022)
Host galaxy properties of quasi-periodically erupting X-ray sources.
Wevers T., Pasham D.R., Jalan P., Rakshit S., Arcodia R.
<Astron. Astrophys. 659, L2 (2022)>
=2022A&A...659L...2W 2022A&A...659L...2W (SIMBAD/NED BibCode)
ADC_Keywords: QSOs ; X-ray sources ; Spectroscopy
Keywords: accretion, accretion disks - galaxies: Seyfert - galaxies: active -
galaxies: nuclei - quasars: supermassive black holes
Abstract:
We perform a systematic study of the five known QPE host galaxies with
the aim of providing new insights into their nature. We analyse new
and archival medium resolution optical spectroscopy of the QPE hosts.
We measure emission (and absorption) line fluxes, their ratios and
equivalent widths (EWs), to locate the QPE hosts on diagnostic
diagrams. We also measure the velocity dispersion of the stellar
absorption lines to estimate their black hole masses. All QPE host
galaxies show emission lines in their optical spectra. Based on their
ratios and EWs, we find evidence for the presence of an active
galactic nucleus in all sources, including those previously reported
as passive. We measure velocity dispersions between 36 and 90km/s,
implying the presence of low mass (105-6.7 solar masses) black
holes, consistent with literature findings. Finally, we find a
significant over-representation (2/5 sources, or a factor of
13+13-10 quiescent Balmer strong (post-starburst) galaxies among
QPE hosts.
Description:
The fits files are the reduced spectra of 4/5 host galaxies presented
in the paper. Three of these were taken with Magellan/MagE (eRO-QPE1,
eRO-QPE2 and GSN069). One was taken with Keck/ESI (2MASXJ0249). The
final spectrum was taken with SDSS (RXJ1301) and can be retrieved from
the SDSS archive.
In addition to these fits files, we also include the
continuum-normalised spectra in ascii format. The line flux and EW
measurements were done on these spectra, except for the Lick Hdelta
index for RXJ1301 and eRO-QPE1, which were done on the raw spectrum
(i.e. not template subtracted).
Objects:
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RA (2000) DE Designation(s)
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01 19 08.659 -34 11 30.544 GSN069 = GSN 69
02 31 47.16 -10 20 10.97 eRO-QPE1
02 34 48.696 -44 19 32.779 eRO-QPE2
02 49 17.318 -04 12 52.128 2MASXJ0249 = 2MASX J02491731-0412521
13 02 00.137 +27 46 57.831 RXJ1301 = RX J1301.9+2746
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File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
gsn069.dat 31 12924 GSN 69 continuum-normalised spectrum
ero-qpe1.dat 31 6850 eRO-QPE1 continuum-normalised spectrum
ero-qpe2.dat 31 12925 eRO-QPE2 continuum-normalised spectrum
rxj1301.dat 31 2707 RX J1301.9+2746 continuum-normalised spectrum
j0249.dat 60 27489 2MASX J02491731-0412521 continuum-normalised
spectrum
list.dat 95 4 List of fits spectra
fits/* . 4 Individual fits spectra
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Byte-by-byte Description of file: rxj1301.dat gsn069.dat ero-qpe?.dat
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Bytes Format Units Label Explanations
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1- 11 F11.6 0.1nm lambda Wavelength array of the spectrum
14- 21 F8.5 --- Flux Template subtracted flux
23- 31 F9.5 --- e_Flux Uncertainty on template subtracted flux
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Byte-by-byte Description of file: j0249.dat
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Bytes Format Units Label Explanations
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4- 21 F18.16 0.1nm lambda Wavelength array of the spectrum
28- 43 E16.8 --- Flux Continuum normalised flux
46- 60 E15.8 --- e_Flux Uncertainty on template subtracted flux
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Byte-by-byte Description of file: list.dat
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Bytes Format Units Label Explanations
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1- 5 I5 --- Nx Number of pixels along X-axis
7- 8 I2 --- Ny Number of pixels along Y-axis
10 I1 --- Nz ? Number of spectra
12- 21 A10 "datime" Obs.date Observation date
23- 25 I3 Kibyte size Size of FITS file
27- 53 A27 --- FileName Name of FITS file, in subdirectory fits
55- 95 A41 --- Title Title of the FITS file (1)
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Note (1): For the Magellan/MagE spectra (eRO-QPE1, eRO-QPE2 and GSN069), the
data can be easily read using the multispec (Python) package.
For each echelle order, the fits files contain 5 arrays:
1. Sum of the sky over the extraction aperture.
2. Sum of the object over the extraction aperture.
3. Expected noise from sum of object and sky plus the read noise.
4. Signal-to-noise spectrum (per pixel).
5. The sum of the lamp spectrum over the extraction aperture.
For more details of the reduction process and resulting data products,
please consult the references in the paper, or the following webpage:
https://code.obs.carnegiescience.edu/mage-pipeline
For the Keck/ESI spectrum (2MASX J02491731-0412521), the fits header contains
all the information necessary to reconstruct the wavelength array
(i.e. the CRVAL1 and CDELT1 keywords), and the location of the data is
indicated in the fits header:
BANDID1 = spectrum
BANDID2 = sky background
BANDID3 = error
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Acknowledgements:
Thomas Wevers, twevers(at)eso.org
(End) Patricia Vannier [CDS] 15-Feb-2022