J/MNRAS/499/4325    AGN contrib. of interac. galaxies     (Ramos Padilla+, 2020)

The AGN contribution to the UV-FIR luminosities of interacting galaxies and its role in identifying the main sequence. Ramos Padilla A.F., Ashby M.L.N., Smith H.A., Martinez-Galarza J.R., Beverage A.G., Dietrich J., Higuera-G. M.-A., Weiner A.S. <Mon. Not. R. Astron. Soc., 499, 4325-4369 (2020)> =2020MNRAS.499.4325R 2020MNRAS.499.4325R (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, photometry; Active gal. nuclei Keywords: techniques: photometric - techniques: spectroscopic - galaxies: active - galaxies: evolution - galaxies: interactions - galaxies: starburst Abstract: Emission from active galactic nuclei (AGNs) is known to play an important role in the evolution of many galaxies including luminous and ultraluminous systems (U/LIRGs), as well as merging systems. However, the extent, duration, and exact effects of its influence are still imperfectly understood, as are the conditions that lead to it dominating the IR emission, and then fading again after coalescence. To assess the impact of AGNs on interacting systems, we present a Spectral Energy Distribution (SED) analysis of a sample of 188 nearby galaxies We gather and systematically re-reduce archival broad-band imaging mosaics from the ultraviolet to the far-infrared using data from GALEX, SDSS, 2MASS, IRAS, WISE, Spitzer, and Herschel. We use spectroscopy from Spitzer/IRS to obtain fluxes from fine-structure lines that trace star formation and AGN activity. Utilizing the SED modelling and fitting tool CIGALE, we derive the physical conditions of the interstellar medium, both in star-forming regions and in nuclear regions dominated by the AGN in these galaxies. We investigate how the star formation rates (SFRs) and the fractional AGN contributions (fAGN) depend on stellar mass, galaxy type, and merger stage. We find that luminous galaxies more massive than about 10^10M* are likely to deviate significantly from the conventional galaxy main-sequence relation. Interestingly, infrared AGN luminosity and stellar mass in this set of objects are much tighter than SFR and stellar mass. We find that buried AGNs may occupy a locus between bright starbursts and pure AGNs in the fAGN-[NeV]/[NeII] plane. We identify a modest correlation between fAGN and mergers in their later stages. Description: We present the basic data, photometry and derived parameters from the four samples of galaxies presented in this work. Tables A1-A4 in the article are cds tables: SIGS, SB, AGN and LSM. Tables A6-A9 are combined in Photometry.cds and Tables A10-A13 are combined in Parameters.cds. Table A14, contains the derived parameters for six AGN galaxies where a different viewing angle was used. File Summary: -------------------------------------------------------------------------------- FileName Lrecl Records Explanations -------------------------------------------------------------------------------- ReadMe 80 . This file tablea1.dat 66 100 Basic data for the SIGS sample galaxies tablea2.dat 61 21 Basic data for the SB sample galaxies tablea3.dat 76 29 Basic data for the AGN sample galaxies tablea4.dat 82 38 Basic data for the LSM sample galaxies photom.dat 500 188 Photometry for all galaxies (tables A6-A9) param.dat 142 178 CIGALE (bayes) derived parameters for all galaxies with good fits (tables A6-A9) parampsi.dat 142 6 CIGALE (bayes) derived parameters for six AGN galaxies with different Psi (tables A10-13) -------------------------------------------------------------------------------- See also: J/ApJS/218/6 : Spitzer Interacting Galaxies Survey (SIGS) (Brassington+, 2015) Byte-by-byte Description of file: tablea1.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 2 I2 --- Grp [1-48] Group ID for the SIGS sample 4- 12 A9 --- Galaxy Galaxy ID 14- 15 I2 h RAh Right ascension (J2000) 17- 18 I2 min RAm Right ascension (J2000) 20- 23 F4.1 s RAs Right ascension (J2000) 25 A1 --- DE- Declination sign (J2000) 26- 27 I2 deg DEd Declination (J2000) 29- 30 I2 arcmin DEm Declination (J2000) 32- 35 F4.1 arcsec DEs Declination (J2000) 37- 42 F6.4 --- z Redshift 44 A1 --- Sample [CA] C or A indicates objects belonging to the Keel-Complete sample or the Arp sample, respectively 46 I1 --- Stage [2/5] Merger stage as defined by Dopita et al. (2002ApJS..143...47D 2002ApJS..143...47D) 48- 52 F5.1 arcsec Size1 Angular size 54 A1 --- --- [x] 56- 60 F5.1 arcsec Size2 Angular size 62- 66 F5.1 deg Angle Inclination angle used in photutils -------------------------------------------------------------------------------- Byte-by-byte Description of file: tablea2.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 8 A8 --- Galaxy Galaxy ID 10- 11 I2 h RAh Right ascension (J2000) 13- 14 I2 min RAm Right ascension (J2000) 16- 19 F4.1 s RAs Right ascension (J2000) 21 A1 --- DE- Declination sign (J2000) 22- 23 I2 deg DEd Declination (J2000) 25- 26 I2 arcmin DEm Declination (J2000) 28- 31 F4.1 arcsec DEs Declination (J2000) 33- 38 F6.4 --- z Redshift 40- 41 A2 --- Sample [BS ] B or S indicates B wheter the objects belong to Brand et al. (2006ApJ...641..140B 2006ApJ...641..140B, Cat. J/ApJ/641/140) or added as well known local starbursts, respectively 43- 47 F5.1 arcsec Size1 Angular size 49 A1 --- --- [x] 51- 55 F5.1 arcsec Size2 Angular size 57- 61 F5.1 deg Angle Inclination angle used in photutils -------------------------------------------------------------------------------- Byte-by-byte Description of file: tablea3.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 21 A21 --- Galaxy Galaxy ID 23- 24 I2 h RAh Right ascension (J2000) 26- 27 I2 min RAm Right ascension (J2000) 29- 32 F4.1 s RAs Right ascension (J2000) 34 A1 --- DE- Declination sign (J2000) 35- 36 I2 deg DEd Declination (J2000) 38- 39 I2 arcmin DEm Declination (J2000) 41- 44 F4.1 arcsec DEs Declination (J2000) 47- 52 F6.4 --- z Redshift 54- 56 A3 --- Sample [GHS R] G, H or S indicates whether objects belong to the GOALS sample (G), Higuera-G. & Ramos P. (2013,HR) or taken from SIMBAD (S), respectively 58- 62 F5.1 arcsec Size1 Angular size 64 A1 --- --- [x] 66- 70 F5.1 arcsec Size2 Angular size 72- 76 F5.1 deg Angle Inclination angle used in photutils -------------------------------------------------------------------------------- Byte-by-byte Description of file: tablea4.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 23 A23 --- Galaxy Galaxy ID 25- 26 I2 h RAh Right ascension (J2000) 28- 29 I2 min RAm Right ascension (J2000) 31- 34 F4.1 s RAs Right ascension (J2000) 36 A1 --- DE- Declination sign (J2000) 37- 38 I2 deg DEd Declination (J2000) 40- 41 I2 arcmin DEm Declination (J2000) 43- 46 F4.1 arcsec DEs Declination (J2000) 48- 53 F6.4 --- z Redshift 55- 59 F5.2 solLum log(LIR) log IR luminosity taken from Wang et al. (2014AJ....148....4W 2014AJ....148....4W, Cat. J/AJ/148/4) 61- 63 F3.1 --- Stage Merger stage as defined by Dopita et al. (2002) 66- 69 F4.1 arcsec Size1 Angular size 71 A1 --- --- [x] 73- 76 F4.1 arcsec Size2 Angular size 78- 82 F5.1 deg Angle Inclination angle used in photutils -------------------------------------------------------------------------------- Byte-by-byte Description of file: photom.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 23 A23 --- Galaxy Galaxy ID 24- 30 F7.3 mJy FUV ? Flux FUV band (GALEX 0.152um) 32- 37 F6.3 mJy e_FUV ? Flux uncertainty FUV band 39- 44 F6.2 mJy NUV ? Flux NUV band (GALEX 0.227um) 46- 50 F5.2 mJy e_NUV ? Flux uncertainty NUV band 52- 58 F7.2 mJy uprime ? Flux u_prime band (SDSS DR12 0.354um) 60- 64 F5.2 mJy e_uprime ? Flux uncertainty u_prime band 66- 72 F7.2 mJy gprime ? Flux g_prime band (SDSS DR12 0.477um) 74- 78 F5.2 mJy e_gprime ? Flux uncertainty g_prime band 80- 86 F7.2 mJy rprime ? Flux r_prime band (SDSS DR12 0.623um) 88- 93 F6.2 mJy e_rprime ? Flux uncertainty r_prime band 95-102 F8.2 mJy iprime ? Flux i_prime band (SDSS DR12 0.762um) 104-109 F6.2 mJy e_iprime ? Flux uncertainty i_prime band 111-118 F8.2 mJy zprime ? Flux z_prime band (SDSS DR12 0.913um) 120-125 F6.2 mJy e_zprime ? Flux uncertainty z_prime band 127-134 F8.2 mJy J2mass ? Flux J_2mass band (2MASS 1.25um) 136-141 F6.2 mJy e_J2mass ? Flux uncertainty J_2mass band 143-150 F8.2 mJy H2mass ? Flux H_2mass band (2MASS 1.65um) 152-157 F6.2 mJy e_H2mass ? Flux uncertainty H_2mass band 159-166 F8.2 mJy Ks2mass ? Flux Ks_2mass band (2MASS 2.17um) 168-173 F6.2 mJy e_Ks2mass ? Flux uncertainty Ks_2mass band 175-182 F8.2 mJy WISE1 ? Flux WISE1 band (WISE 3.4um) 184-189 F6.2 mJy e_WISE1 ? Flux uncertainty WISE1 band 191-198 F8.2 mJy IRAC1 ? Flux IRAC1 band (IRAC 3.6um) 200-205 F6.2 mJy e_IRAC1 ? Flux uncertainty IRAC1 band 207-214 F8.2 mJy IRAC2 ? Flux IRAC2 band (IRAC 4.5um) 216-221 F6.2 mJy e_IRAC2 ? Flux uncertainty IRAC2 band 223-230 F8.2 mJy WISE2 ? Flux WISE2 band (WISE 4.5um) 232-237 F6.2 mJy e_WISE2 ? Flux uncertainty WISE2 band 239-246 F8.2 mJy IRAC3 ? Flux IRAC3 band (IRAC 5.8um) 248-253 F6.2 mJy e_IRAC3 ? Flux uncertainty IRAC3 band 255-262 F8.2 mJy IRAC4 ? Flux IRAC4 band (IRAC 8.0um) 264-270 F7.2 mJy e_IRAC4 ? Flux uncertainty IRAC4 band 272-279 F8.2 mJy IRAS1 ? Flux IRAS1 band (IRAS 12um) 281-287 F7.2 mJy e_IRAS1 ? Flux uncertainty IRAS1 band 289-296 F8.2 mJy WISE3 ? Flux WISE3 band (WISE 12um) 298-305 F8.2 mJy e_WISE3 ? Flux uncertainty WISE3 band 307-314 F8.2 mJy WISE4 ? Flux WISE4 band (WISE 22um) 316-323 F8.2 mJy e_WISE4 ? Flux uncertainty WISE4 band 325-332 F8.2 mJy MIPS1 ? Flux MIPS1 band (MPIS 24um) 334-341 F8.2 mJy e_MIPS1 ? Flux uncertainty MIPS1 band 343-351 F9.2 mJy IRAS2 ? Flux IRAS2 band (IRAS 25um) 353-360 F8.2 mJy e_IRAS2 ? Flux uncertainty IRAS2 band 362-368 F7.2 Jy IRAS3 ? Flux IRAS3 band (IRAS 60um) 370-374 F5.2 Jy e_IRAS3 ? Flux uncertainty IRAS3 band 376-382 F7.2 Jy PACSblue ? Flux PACS_blue band (PACS 70um) 384-389 F6.2 Jy e_PACSblue ? Flux uncertainty PACS_blue band 391-396 F6.2 Jy MIPS2 ? Flux MIPS2 band (MIPS 70um) 398-402 F5.2 Jy e_MIPS2 ? Flux uncertainty MIPS2 band 404-410 F7.2 Jy IRAS4 ? Flux IRAS4 band (IRAS 100um) 412-417 F6.2 Jy e_IRAS4 ? Flux uncertainty IRAS4 band 419-425 F7.2 Jy PACSgreen ? Flux PACS_green band (PACS 100um) 427-432 F6.2 Jy e_PACSgreen ? Flux uncertainty PACS_green band 434-439 F6.2 Jy MIPS3 ? Flux MIPS3 band (MIPS 160um) 441-445 F5.2 Jy e_MIPS3 ? Flux uncertainty MIPS3 band 447-453 F7.2 Jy PACSred ? Flux PACS_red band (PACS 180um) 455-460 F6.2 Jy e_PACSred ? Flux uncertainty PACS_red band 462-467 F6.2 Jy PSW ? Flux PSW_ext band (SPIRE 250um) 469-473 F5.2 Jy e_PSW ? Flux uncertainty PSW_ext band 475-480 F6.2 Jy PMW ? Flux PMW_ext band (SPIRE 350um) 482-486 F5.2 Jy e_PMW ? Flux uncertainty PMW_ext band 488-494 F7.3 Jy PLW ? Flux PLW_ext band (SPIRE 500um) 496-500 F5.3 Jy e_PLW ? Flux uncertainty PLW_ext band -------------------------------------------------------------------------------- Byte-by-byte Description of file: param.dat parampsi.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 23 A23 --- Galaxy Galaxy ID 25- 28 F4.2 --- agn.fAGN AGN fraction 30- 33 F4.2 --- e_agn.fAGN AGN fraction error 35- 39 F5.2 [Lsun] agn.lum log AGN luminosity of the three AGN components by Fritz et al. (2006MNRAS.366..767F 2006MNRAS.366..767F) 41- 44 F4.2 [Lsun] e_agn.lum log AGN luminosity error of the three components by Fritz et al. (2006MNRAS.366..767F 2006MNRAS.366..767F) 46- 50 F5.2 [Lsun] att.stel.old log old attenuation from the old stellar population 52- 55 F4.2 [Lsun] e_att.stel.old log old attenuation error from the old stellar population 57- 61 F5.2 [Lsun] att.stel.young log young attenuation from the old stellar population 63- 67 F5.2 [Lsun] e_att.stel.young log young attenuation error from the old stellar population 69- 72 F4.2 --- dust.alpha Parameter that defines the contribution of the local heating intensity in the dust 74- 77 F4.2 --- e_dust.alpha Error on dust.alpha 79- 83 F5.2 [Lsun] dust.lum log dust luminosity 85- 88 F4.2 [Lsun] e_dust.lum log dust luminosity error 90- 94 F5.2 [Msun/yr] sfh.sfr log star formation rate 96-100 F5.2 [Msun/yr] e_sfh.sfr log star formation rate error 102-105 F4.2 [yr] sfh.tau-main log e-folding time of the main stellar population model 107-110 F4.2 [yr] e_sfh.tau-main log e-folding time of the main stellar population model error 112-115 F4.2 [yr] stel.age.m-star log age of the oldest stars in the galaxy 117-120 F4.2 [yr] e_stel.age.m-star log age of the oldest stars in the galaxy error 122-126 F5.2 [Msun] stel.m-gas log gas mass 128-131 F4.2 [Msun] e_stel.m-gas log gas mass error 133-137 F5.2 [Msun] stel.m-star log stellar mass 139-142 F4.2 [Msun] e_stel.m-star log stellar mass error -------------------------------------------------------------------------------- Acknowledgements: Andres Felipe Ramos Padilla, ramos(at)astro.rug.nl
(End) Patricia Vannier [CDS] 26-Nov-2020
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