J/A+A/631/A118 Emission-line sources MUSE spectral catalogue (Goettgens+, 2019)
A stellar census in globular clusters with MUSE:
A spectral catalogue of emission-line sources.
Goettgens F., Husser T.-O., Kamann S., Dreizler S., Giesers B.,
Kollatschny W., Weilbacher P.M., Roth M.M., Wendt M.
<Astron. Astrophys. 631, A118 (2019)>
=2019A&A...631A.118G 2019A&A...631A.118G (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, globular ; Stars, emission ; Spectrophotometry
Keywords: globular clusters: general - stars: emission-line, Be -
novae, cataclysmic variables - catalogs -
techniques: imaging spectroscopy
Abstract:
Globular clusters produce many exotic stars due to a much higher
frequency of dynamical interactions in their dense stellar
environments.
Some of these objects were observed together with several hundred
thousand other stars in our MUSE survey of 26 Galactic globular
clusters.
Assuming that at least a few exotic stars have exotic spectra (i.e.
spectra that contain emission lines), we can use this large
spectroscopic data set of over a million stellar spectra as a blind
survey to detect stellar exotica in globular clusters.
To detect emission lines in each spectrum, we modelled the expected
shape of an emission line as a Gaussian curve.
This template was used for matched filtering on the differences
between each observed 1D spectrum and its fitted spectral model.
The spectra with the most significant detections of Hα emission
are checked visually and cross-matched with published catalogues.
We find 156 stars with Hα emission, including several known
cataclysmic variables (CV) and two new CVs, pulsating variable stars,
eclipsing binary stars, the optical counterpart of a known black hole,
several probable sub-subgiants and red stragglers, and 21 background
emission-line galaxies.
We find possible optical counterparts to 39 X-ray sources, as we
detected H_alpha emission in several spectra of stars that are close
to known positions of Chandra X-ray sources.
This spectral catalogue can be used to supplement existing or future
X-ray or radio observations with spectra of potential optical
counterparts to classify the sources.
Description:
The spectra were extracted from datacubes taken with MUSE at the VLT.
We used matched filtering to search for emission-line objects (ELOs)
in globular clusters. The tables contain the properties of the
detected ELOs, including references to the literature. Please see the
paper for details about which filter was used for the reported V
magnitude, and which conventions are used for the cluster membership
indicator and the indicator for radial velocity variations.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea2.dat 153 156 ELO properties
list.dat 109 1454 List of fits spectra
fits/* . 1454 Individual fits spectra
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Byte-by-byte Description of file: tablea2.dat
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Bytes Format Units Label Explanations
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1- 7 A7 --- Cluster Cluster name
9- 19 F11.7 deg RAdeg Right ascension (J2000)
21- 31 F11.7 deg DEdeg Declination (J2000)
33- 39 I7 --- ACS ACS Survey ID
41- 45 F5.1 arcsec CenDist Distance to center
47- 50 F4.1 mag Vmag V magnitude
52- 54 A3 --- Memb [yes/no/unc ] Cluster membership indicator
56- 58 A3 km/s RV [yes/no/unc ] Variable RV indicator
60- 63 F4.2 arcsec DX ? Distance to next Xray source (if close)
65-125 A61 --- Comment Comment
127-147 A21 --- Ident Identification
149-153 A5 --- Ref Reference for identification (1)
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Note (1): References as follows:
1 = Heinke et al. (2005, Cat. J/ApJ/625/796)
2 = Clement et al. (2001AJ....122.2587C 2001AJ....122.2587C, Cat. V/150)
3 = Albrow et al. (2001, Cat. J/ApJ/559/1060)
4 = Kunder et al. (2013AJ....145...33K 2013AJ....145...33K)
5 = Kaluzny et al. (2016AcA....66...31K 2016AcA....66...31K)
6 = Lebzelter & Wood (2016, Cat. J/A+A/585/A111)
7 = Cool et al. (2013ApJ...763..126C 2013ApJ...763..126C)
8 = Heinke et al. (2003ApJ...598..516H 2003ApJ...598..516H)
9 = Dieball et al. (2010, Cat. J/ApJ/710/332)
10 = Bassa et al. (2004ApJ...609..755B 2004ApJ...609..755B)
11 = Lu et al. (2009, Cat. J/A+A/585/A111)
12 = Chomiuk et al. (2013ApJ...777...69C 2013ApJ...777...69C)
13 = Webb et al. (2004A&A...424..133W 2004A&A...424..133W)
14 = Pooley et al. (2002ApJ...569..405P 2002ApJ...569..405P)
15 = Lugger et al. (2017ApJ...841...53L 2017ApJ...841...53L)
16 = Lugger et al. (2007ApJ...657..286L 2007ApJ...657..286L)
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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- 4 I4 --- Nx Number of pixels along X-axis
6- 28 A23 "datime" Obs.date Observation date
30- 40 E11.6 0.1nm bAWAV Lower value of wavelength interval
42- 52 E11.6 0.1nm BAWAV Upper value of wavelength interval
54- 61 E8.3 0.1nm dAWAV ? Wavelength resolution
63- 64 I2 Kibyte size Size of FITS file
66- 89 A24 --- FileName Name of FITS file, in subdirectory fits
91- 97 A7 --- Cluster Cluster name
99-105 I7 --- ACS ACS Survey ID
107-109 I3 --- Specid Running ID for spectrum,
999 = combined spectrum
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Acknowledgements:
Fabian Goettgens, fabian.goettgens(at)uni-goettingen.de
References:
Sarajedini et al., 2007AJ....133.1658S 2007AJ....133.1658S ACS survey of galactic globular clusters
(End) Patricia Vannier [CDS] 25-Sep-2019