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J/MNRAS/459/2948    Ccompact group galaxies UV and IR SFR    (Lenkic+, 2016)

The ultraviolet and infrared star formation rates of compact group galaxies: an expanded sample. Lenkic L., Tzanavaris P., Gallagher S.C., Desjardins T.D., Walker L.M., Johnson K.E., Fedotov K., Charlton J., Hornschemeier A.E., Durrell P.R., Gronwall C. <Mon. Not. R. Astron. Soc., 459, 2948-2963 (2016)> =2016MNRAS.459.2948L (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, galaxy ; Galaxies, photometry ; Photometry, infrared ; Photometry, ultraviolet Keywords: galaxies: evolution - galaxies: photometry - galaxies: star formation Abstract: Compact groups of galaxies provide insight into the role of low-mass, dense environments in galaxy evolution because the low velocity dispersions and close proximity of galaxy members result in frequent interactions that take place over extended time-scales. We expand the census of star formation in compact group galaxies by Tzanavaris et al. (2010, Cat. J/ApJS/212/9) and collaborators with Swift UVOT, Spitzer IRAC and MIPS 24µm photometry of a sample of 183 galaxies in 46 compact groups. After correcting luminosities for the contribution from old stellar populations, we estimate the dust-unobscured star formation rate (SFRUV) using the UVOT uvw2 photometry. Similarly, we use the MIPS 24 µm photometry to estimate the component of the SFR that is obscured by dust (SFRIR). We find that galaxies which are MIR-active (MIR-'red'), also have bluer UV colours, higher specific SFRs, and tend to lie in HI-rich groups, while galaxies that are MIR-inactive (MIR-'blue') have redder UV colours, lower specific SFRs, and tend to lie in HI-poor groups. We find the SFRs to be continuously distributed with a peak at about 1M/yr, indicating this might be the most common value in compact groups. In contrast, the specific SFR distribution is bimodal, and there is a clear distinction between star-forming and quiescent galaxies. Overall, our results suggest that the specific SFR is the best tracer of gas depletion and galaxy evolution in compact groups. Description: The sample of CGs studied here is the same sample studied by Walker et al. (2012AJ....143...69W) of 49 CGs: 33 Hickson Compact Groups and 16 Redshift Survey Compact Groups (RSCGs). The RSCG catalogue of 89 CGs was constructed by Barton et al. (1996AJ....112..871B). The data used in this study originated from 'fill-in' observations with UVOT's three UV filters (uvw2, uvm2, uvw1) as well as the bluest optical filter (u). All UV data (PI: Tzanavaris) were downloaded from the Swift archive. The Spitzer Infrared Array Camera images for our sample of CGs are archival data presented by Walker et al. (2012AJ....143...69W) Spitzer MIPS (24um) data were obtained from the Spitzer Heritage Archive. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file groups.dat 32 43 Studied groups table3.dat 80 217 Observation log for Swift UVOT HCG and RSCG data table5.dat 126 174 UVOT, MIPS 24um and IRAC 3.6 and 4.5um fluxes for HCG and RSCG galaxies table6.dat 77 169 UV and IR properties of HCG and RSCG galaxies
See also: J/ApJS/212/9 : X-ray sources in Hickson Compact Groups (Tzanavaris+, 2014) Byte-by-byte Description of file: groups.dat
Bytes Format Units Label Explanations
1- 7 A7 --- Group Group name 10- 11 I2 h RAh Simbad right ascension (J2000) 13- 14 I2 min RAm Simbad right ascension (J2000) 16- 20 F5.2 s RAs Simbad right ascension (J2000) 22 A1 --- DE- Simbad declination sign (J2000) 23- 24 I2 deg DEd Simbad declination (J2000) 26- 27 I2 arcmin DEm Simbad declination (J2000) 29- 32 F4.1 arcsec DEs ? Simbad declination (J2000)
Byte-by-byte Description of file: table3.dat
Bytes Format Units Label Explanations
1- 7 A7 --- Group Group ID 9- 19 I11 --- ObsID Observation ID 21- 52 A32 --- Obs.Date Dates of Observations 53- 57 I5 s ExpTUVW2 ? Total Exposure Times for Swift UVOT filter UVW2 61- 65 I5 s ExpTUVM2 ? Total Exposure Times for Swift UVOT filter UVM2 69- 73 I5 s ExpTUVW1 ? Total Exposure Times for Swift UVOT filter UVW1 76- 80 I5 s ExpTU ? Total Exposure Times for Swift UVOT filter U
Byte-by-byte Description of file: table5.dat
Bytes Format Units Label Explanations
1- 10 A10 --- CGG Compact Group Galaxy name 11- 16 F6.1 10-19W/m2 FUVW2 ?=- UVOT UVW2 flux density 18- 21 F4.1 10-19W/m2 e_FUVW2 ? rms uncertainty on FUVW2 23 A1 --- l_FUVW2c Limit flag on FUVW2c 24- 30 F7.3 10-19W/m2 FUVW2c ?=- UVOT UVW2 flux density corrected for emission from old stellar populations 32- 37 F6.1 10-19W/m2 FUVM2 ?=- UVOT UVM2 flux density 39- 42 F4.1 10-19W/m2 e_FUVM2 ? rms uncertainty on FUVM2 44- 49 F6.1 10-19W/m2 FUVW1 ?=- UVOT UVW1 flux density 51- 54 F4.1 10-19W/m2 e_FUVW1 ? rms uncertainty on FUVW1 57- 62 F6.1 10-19W/m2 FU ?=- UVOT U flux density 64- 67 F4.1 10-19W/m2 e_FU ? rms uncertainty on FU 68- 70 A3 --- n_FU [(b)] Note on FU (1) 73- 76 F4.1 mag UVM2mag ?=- UVM2 AB magnitude 79- 83 F5.1 mJy F3.6 ?=- IRAC 3.6um flux density 85- 88 F4.1 mJy e_F3.6 ?=- rms uncertainty on F3.6 90- 94 F5.1 mJy F4.5 ?=- IRAC 4.5um flux density 96- 99 F4.1 mJy e_F4.5 ?=- rms uncertainty on F4.5 101-106 F6.1 mJy F24 ?=- MIPS 24um flux density 108-112 F5.1 mJy e_F24 ? rms uncertainty on F24 114 A1 --- l_F24c Limit flag on F24c 115-120 F6.1 mJy F24c ?=- 24 micron flux density corrected for emission from old stellar populations 122-126 F5.1 mJy e_F24c ? rms uncertainty on F24c
Note (1): (b) : We checked our UV data for coincidence loss effects using the method of Poole et al. (2008MNRAS.383..627P), by measuring the non-background subtracted count rates in circular apertures within a 5 arcsec radius centred on the surface brightness peak. Consistent with the results of Tzanavaris et al. (2010ApJ...716..556T), we found that the U filter images were most significantly affected by coincidence loss; 32 of 120 galaxies with U data suffered from coincidence loss, whereas only 6, 2, and 5 galaxies suffered from coincidence loss effects in the UVW1, UVM2, and UVW2 filters, respectively.
Byte-by-byte Description of file: table6.dat
Bytes Format Units Label Explanations
1 A1 --- Case [A/Q] Case (1) 3- 12 A10 --- CGG Compact Group Galaxy name 14- 15 A2 --- MType Galaxy Morphology (2) 17- 21 F5.2 [10-7W/Hz] logLUVW2 ?=- UVOT UVW2 luminosity 23- 27 F5.2 [10-7W/Hz] logLUVM2 ?=- UVOT UVM2 luminosity 29- 33 F5.2 [10-7W/Hz] logLUVW1 ?=- UVOT UVM1 luminosity 35- 39 F5.2 [10-7W/Hz] logLU ? UVOT U luminosity 41- 45 F5.2 [10-7W/Hz] logL24 ? MIPS 24um luminosity 47- 51 F5.2 [Msun] logM* ?=- Stellar mass 53- 57 F5.2 --- alphaIRAC ? alphaIRAC parameter, obtained from Dejardins et al. (2015, AAS Meeting, 225, 321.02) 59- 63 F5.3 --- SFRuvw2 ?=- UV component of the star formation rate 65- 70 F6.3 --- SFR24um ?=- IR component of the total star formation 72- 77 F6.3 10-11 SSFR ?=- Specific star formation rate (3)
Note (1): Case as follows: A = Actively Star Forming (alphaIRAC≤0) Q = Quiescent (alphaIRAC>0) Note (2): Morphology of each galaxy, obtained from Tyler Desjardins, priv. comm., Note (3): Specific star formation rate, which is the total star formation rate, normalized by stellar mass.
History: From electronic version of the journal
(End) Patricia Vannier [CDS] 28-Jul-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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