NASA/IPAC EXTRAGALACTIC DATABASE
Date and Time of the Query: 2019-08-17 T16:33:35 PDT
Help | Comment | NED Home

For refcode 2014A&A...568A..62D:
Retrieve 469 NED objects in this reference.
Please click here for ADS abstract

NED Abstract

Copyright by European Southern Observatory (ESO). Reproduced by permission
2014A&A...568A..62D The applicability of far-infrared fine-structure lines as star formation rate tracers over wide ranges of metallicities and galaxy types De Looze, Ilse; Cormier, Diane; Lebouteiller, Vianney; Madden, Suzanne; Baes, Maarten; Bendo, George J.; Boquien, Mederic; Boselli, Alessandro; Clements, David L.; Cortese, Luca; Cooray, Asantha; Galametz, Maud; Galliano, Frederic; Gracia-Carpio, Javier; Isaak, Kate; Karczewski, Oskar L.; Parkin, Tara J.; Pellegrini, Eric W.; Remy-Ruyer, Aurelie; Spinoglio, Luigi; Smith, Matthew W. L.; Sturm, Eckhard Abstract. Aims: We analyze the applicability of far-infrared fine-structure lines [Cii] 158 micron, [Oi] 63 micron, and [Oiii] 88 micron to reliably trace the star formation rate (SFR) in a sample of low-metallicity dwarf galaxies from the Herschel Dwarf Galaxy Survey and, furthermore, extend the analysis to a broad sample of galaxies of various types and metallicities in the literature. Methods: We study the trends and scatter in the relation between the SFR (as traced by GALEX FUV and MIPS 24 micron) and far-infrared line emission, on spatially resolved and global galaxy scales, in dwarf galaxies. We assemble far-infrared line measurements from the literature and infer whether the far-infrared lines can probe the SFR (as traced by the total infrared luminosity) in a variety of galaxy populations. Results: In metal-poor dwarfs, the [Oi]_63_ and [Oiii]_88_ lines show the strongest correlation with the SFR with an uncertainty on the SFR estimates better than a factor of 2, while the link between [Cii] emission and the SFR is more dispersed (uncertainty factor of 2.6). The increased scatter in the SFR-L_[CII]_ relation toward low metal abundances, warm dust temperatures, and large filling factors of diffuse, highly ionized gas suggests that other cooling lines start to dominate depending on the density and ionization state of the gas. For the literature sample, we evaluate the correlations for a number of different galaxy populations. The [Cii] and [Oi]_63_ lines are considered to be reliable SFR tracers in starburst galaxies, recovering the star formation activity within an uncertainty of factor 2. For sources with composite and active galactic nucleus (AGN) classifications, all three FIR lines can recover the SFR with an uncertainty factor of 2.3. The SFR calibrations for ultra-luminous infrared galaxies (ULIRGs) are similar to starbursts/AGNs in terms of scatter but offset from the starburst/AGN SFR relations because of line deficits relative to their total infrared luminosity. While the number of detections of the FIR fine-structure lines is still very limited at high redshift for [Oi]_63_ and [Oiii]_88_, we provide an SFR calibration for [Cii]. Key words: Galaxy: abundances, galaxies: dwarf, galaxies: ISM, galaxies: star formation
Retrieve 469 NED objects in this reference.
Please click here for ADS abstract

Back to NED Home