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J/A+A/607/A110      AMIGA sample: CO properties              (Lisenfeld+, 2017)

The role of molecular gas in galaxy transition in compact groups. Lisenfeld U., Alatalo K., Zucker C., Appleton P.N., Gallagher S., Guillard P., Johnson K. <Astron. Astrophys. 607, A110 (2017)> =2017A&A...607A.110L (SIMBAD/NED BibCode)
ADC_Keywords: Carbon monoxide ; Galaxies, IR ; Interstellar medium Keywords: ISM: molecules - galaxies: interactions - galaxies: evolution - galaxies: ISM - galaxies: star formation - galaxies: groups: general Abstract: Compact groups (CGs) provide an environment in which interactions between galaxies and with the intra-group medium enable and accelerate galaxy transitions from actively star forming to quiescent. Galaxies in transition from active to quiescent can be selected, by their infrared (IR) colors, as canyon or infrared transition zone (IRTZ) galaxies. We used a sample of CG galaxies with IR data from the Wide Field Infrared Survey Explorer (WISE) allowing us to calculate the stellar mass and star formation rate (SFR) for each galaxy. Furthermore, we present new CO(1-0) data for 27 galaxies and collect data from the literature to calculate the molecular gas mass for a total sample of 130 galaxies. This data set allows us to study the difference in the molecular gas fraction (Mmol/Mstar) and star formation efficiency (SFE=SFR/Mmol) between active, quiescent, and transitioning (i.e., canyon and IRTZ) galaxies. We find that transitioning galaxies have a mean molecular gas fraction and a mean SFE that are significantly lower than those of actively star-forming galaxies. The molecular gas fraction is higher than that of quiescent galaxies, whereas the SFE is similar. These results indicate that the transition from actively star-forming to quiescent in CG galaxies goes along with a loss of molecular gas, possibly due to tidal forces exerted from the neighboring galaxies or a decrease in the gas density. In addition, the remaining molecular gas loses its ability to form stars efficiently, possibly owing to turbulence perturbing the gas, as seen in other, well-studied examples such as Stephan's Quintet and HCG 57. Thus, the amount and properties of molecular gas play a crucial role in the environmentally driven transition of galaxies from actively star forming to quiescent. Description: Our sample is based on the catalog of Zucker et al. (2016, Cat. J/ApJ/821/113), which presents WISE data for 652 galaxies in 163 compact groups, of which 428 galaxies have reliable photometry (S/N> 2 in all bands). We searched the literature for all existing CO data for this Zucker et al. (2016, Cat. J/ApJ/821/113) subsample (294 galaxies) and obtained CO measurements for 102 HCG galaxies (Verdes-Montenegro et al., 1998ApJ...497...89V; Leon et al., 1998A&A...330...37L; Martinez-Badenes et al., 2012, Cat. J/A+A/540/A96; Lisenfeld et al., 2014, Cat. J/A+A/570/A24) and for two RSCG galaxies (Mirabel et al., 1990A&A...236..327M; Wiklind et al., 1995A&A...297..643W, NGC 232 and NGC 2831). The observations were carried out with the Institut de Radioastronomie Millimetrique (IRAM) 30m telescope, Five College Radio Telescope, Swedish-ESO Submillimetre Telescope (SEST), and Kitt Peak Radio Telescope with single pointings at the central position for most cases. To supplement the CO data for these 104 galaxies from the literature, as part of this study we observed the redshifted CO(1-0) line for an additional 27 galaxies. We observed an additional 27 galaxies in CGs between January and April 2017 with the IRAM 30m telescope on Pico Veleta. We selected the sources, based on their WISE colors, as preferentially canyon or IRTZ objects. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table2.dat 49 130 Molecular gas, SFR and stellar mass
See also: J/A+A/534/A102 : AMIGA IX. Molecular gas properties (Lisenfeld+, 2011) J/A+A/540/A96 : Molecular gas in HCG (Martinez-Badenes+, 2012) J/A+A/570/A24 : CO in HCG galaxies with enhanced warm H2 (Lisenfeld+, 2014) J/ApJ/821/113 : HCG and RSCG compact group galaxies with WISE (Zucker+, 2016) Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 13 A13 --- Name Name of the galaxy 15- 19 F5.1 Mpc Dist Distance (based on H0=70km/s/Mpc) 21 A1 --- l_logMmol0 Upper limit code for logMmol0 (2) 23- 27 F5.2 [Msun] logMmol0 Decimal logarithm of the molecular gas mass in the central pointing 29 A1 --- l_logMmol Upper limit code for logMmol (2) 31- 35 F5.2 [Msun] logMmol Decimal logarithm of the molecular gas mass extrapolated to the entire disk 37 I1 --- Ref Reference code for the CO measurement from which Mmol is calculated (1) 39- 43 F5.2 Msun/yr SFR Star formation rate 45- 49 F5.2 [Msun] logMstar Decimal logarithm of the stellar mass
Note (1): Reference codes for the CO measurement from which Mmol is calculated as follows: 1 = This paper. 2 = Lisenfeld et al. (2014, Cat. J/A+A/534/A102) 3 = Martinez-Badenes et al. (2012, Cat. J/A+A/540/A96) 4 = Leon et al. (1998A&A...330...37L) 5 = Verdes-Montenegro et al. (2001A&A...377..812V) 6 = Wiklind et al. (1995A&A...297..643W) 7 = Mirabel et al. (1990A&A...236..327M) Note (2): Upper limit code for logMol0 and logMol: < for upper limit, else detection
Acknowledgements: Ute Lisenfeld, ute(at)ugr.es
(End) Ute Lisenfeld [Universidad Granada], Patricia Vannier [CDS] 04-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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