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J/MNRAS/459/4450    Peculiar compact stellar systems in Fornax (Wittmann+, 2016)

Peculiar compact stellar systems in the Fornax cluster. Wittmann C., Lisker T., Pasquali A., Hilker M., Grebel E.K. <Mon. Not. R. Astron. Soc., 459, 4450-4466 (2016)> =2016MNRAS.459.4450W (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, galaxy ; Radial velocities ; Morphology Keywords: galaxies: clusters: individual: Fornax - galaxies: dwarf - galaxies: nuclei; galaxies: peculiar - galaxies: star clusters: general - galaxies: structure Abstract: We search for hints to the origin and nature of compact stellar systems in the magnitude range of ultracompact dwarf galaxies in deep wide-field imaging data of the Fornax cluster core. We visually investigate a large sample of 355 spectroscopically confirmed cluster members with V-band equivalent magnitudes brighter than -10mag for faint extended structures. Our data reveal peculiar compact stellar systems, which appear asymmetric or elongated from their outer light distribution. We characterize the structure of our objects by quantifying their core concentration, as well as their outer asymmetry and ellipticity. For the brighter objects of our sample we also investigate their spatial and phase-space distribution within the cluster. We argue that the distorted outer structure alone that is seen for some of our objects, is not sufficient to decide whether these systems have a star cluster or a galaxy origin. However, we find that objects with low core concentration and high asymmetry (or high ellipticity) are primarily located at larger cluster-centric distances as compared to the entire sample. This supports the hypothesis that at least some of these objects may originate from tidally stripped galaxies. Description: The data are fully characterized by Lisker et al. (2016, A&A, submitted). They were acquired in 2008 and 2010 with the WFI at the ESO/MPG 2.2m telescope (programmes 082.A-9016 and 084.A-9014, PI A. Pasquali, Guaranteed Time of the Max Planck Institute for Astronomy). We used a transparent filter that nearly equals the no-filter throughput (>10 per cent in the range 350-900nm) and thus provides a high signal-to-noise ratio. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 69 904 Compilation of compact stellar systems known to be Fornax cluster members, based on previous publications table3.dat 71 355 Parameter catalogue for the working sample of spectroscopically confirmed Fornax cluster members with mVe<21.5mag
Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 3 I3 --- Seq [1/904] Sequential number 5- 6 I2 h RAh Right ascension (J2000) 8- 9 I2 min RAm Right ascension (J2000) 11- 15 F5.2 s RAs Right ascension (J2000) 17 A1 --- DE- Declination sign (J2000) 18- 19 I2 deg DEd Declination (J2000) 21- 22 I2 arcmin DEm Declination (J2000) 24- 27 F4.1 arcsec DEs Declination (J2000) 29- 57 A29 --- Simbad Object identifier of the SIMBAD database, referring to the publication the object was taken from 59- 62 I4 km/s HV Heliocentric velocity with the smallest error from all compiled velocities for an object 64- 66 I3 km/s e_HV rms uncertainty in HV 68- 69 I2 --- r_HV Literature source for the adopted velocity (1)
Note (1): References as follows: 1 = Schuberth et al. (2010, Cat. J/A+A/513/A52) 2 = Dirsch et al. (2004, Cat. J/AJ/127/2114) 3 = Bergond et al. (2007, Cat. J/A+A/464/L21) 4 = Firth et al. (2007, Cat. J/MNRAS/382/1342) 5 = Gregg et al. (2009, Cat. J/AJ/137/498) 6 = Mieske et al. (2004, Cat. J/A+A/418/445) 7 = Mieske et al. (2002, Cat. J/A+A/383/823) 8 = Firth et al. (2008MNRAS.389.1539F) 9 = Kissler-Patig et al. (1999AJ....117.1206K) 10 = Drinkwater et al. (2000PASA...17..227D) 11 = Kissler-Patig et al. (1998AJ....115..105K)
Byte-by-byte Description of file: table3.dat
Bytes Format Units Label Explanations
1- 3 I3 ---- Seq [1/904] Sequential number 5- 10 F6.3 mag Vemag Apparent V-equivalent magnitude 12- 16 F5.3 mag e_Vemag rms uncertainty on Vemag 18 I1 --- f_Vemag [1/2] Magnitude flag (1) 20- 24 F5.3 --- CC Core concentration (uncorrected values) 26- 30 F5.3 --- CCcorr PSF-corrected core concentration 32- 38 F7.3 --- RA ?=-99 Residual asymmetry 40- 46 F7.3 --- e_RA ?=-99 rms uncertainty on RA 48- 54 F7.3 --- Ell ?=-99 Ellipticity 56- 62 F7.3 --- e_Ell ?=-99 rms uncertainty on Ell 64- 65 I2 --- Sub ? Subsample (2) 67- 68 I2 --- SubAlt ? Alternative subsample (2) 70- 71 I2 --- Region PSF-region of the object
Note (1): Magnitude flag as follows: 1 = mag and e_mag obtained from SExtractor 2 = mag and e_mag obtained from PSF-fitting Note (2): Subsamples as follows: 1 = cc+ra 2 = cc+RA 3 = CC+RA 4 = cc+EL 0 = SUB: object not part of any subsample
History: From electronic version of the journal
(End) Patricia Vannier [CDS] 27-Sep-2017
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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