A Compendium of Far-Infrared Line and Continuum Emission for 227 Galaxies Observed by the Infrared Space Observatory

By J. Brauher, D. Dale, G. Helou. 2008

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Far-infrared line and continuum fluxes are presented for a sample of 227 galaxies observed with the Long Wavelength Spectrometer on the Infrared Space Observatory. The galaxy sample includes normal star-forming systems, starbursts, and active galactic nuclei covering a wide range of colors and morphologies. The data set spans some 1300 line fluxes, 600 line upper limits, and 800 continuum fluxes. Several fine-structure emission lines are detected that arise in either photodissociation or H II regions: [O III] 52 μm, [N III] 57 μm, [O I] 63 μm, [O III] 88 μm, [N II] 122 μm, [O I] 145 μm, and [C II] 158 μm. Molecular lines such as OH at 53, 79, 84, 119, and 163 μm, and H2O at 58, 66, 75, 101, and 108 μm are also detected in some galaxies. In addition to those lines emitted by the target galaxies, serendipitous detections of Milky Way [C II] 158 μm and an unidentified line near 74 μm in NGC 1068 are also reported. Finally, continuum fluxes at 52, 57, 63, 88, 122, 145, 158, and 170 μm are derived for a subset of galaxies in which the far-infrared emission is contained within the ~75″ ISO LWS beam. The statistics of this large database of continuum and line fluxes, including trends in line ratios with the far-infrared color and infrared-to-optical ratio, are explored.

Subfields: Astronomy and Astrophysics, Spectroscopy

View Paper: https://www.semanticscholar.org/paper/e00b1e3de0e65ebaac752c5f647de8a3fba41725

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EXPLAINING THE [C ii]157.7 μm DEFICIT IN LUMINOUS INFRARED GALAXIES—FIRST RESULTS FROM A HERSCHEL/PACS STUDY OF THE GOALS SAMPLE (2013, methodology): “…ISO data already suggested that the relative contribution of the [C ii]157.7µm line to the cooling of the ISM in PDRs compared to that of large dust grains, as gauged by the far-IR emission, diminishes as galaxies are more IR luminous (Malhotra et al. 1997; Luhman et al. 1998; Brauher et al. 2008).”
A 158 μm [C ii] LINE SURVEY OF GALAXIES AT z ∼ 1–2: AN INDICATOR OF STAR FORMATION IN THE EARLY UNIVERSE (2010, background): “For most star-forming galaxies, the [O iii] 52 μm/[O iii] 88 μm line ratio is ∼2 (Brauher et al. 2008), which indicates ionized gas densities ∼300 cm−3.”
An Overview of the Dwarf Galaxy Survey (2013, background): “…have been detected in low metallicity dwarf galaxies with the Kuiper Airborne Observatory (KAO) and the ISO LWS (Stacey et al. 1991; Poglitsch et al. 1995; Madden et al. 1997; Madden 2000; Bergvall et al. 2000; Hunter et al. 2001; Vermeij et al. 2002; Brauher et al. 2008; Israel & Maloney 2011).”
THE PdBI ARCSECOND WHIRLPOOL SURVEY (PAWS). I. A CLOUD-SCALE/MULTI-WAVELENGTH VIEW OF THE INTERSTELLAR MEDIUM IN A GRAND-DESIGN SPIRAL GALAXY (2013, background): “The strongest far-IR cooling line of the cold ISM in nearby galaxies is [CII] at 158µm which can contain up to 1% of the total far-IR luminosity (Stacey et al. 1991; Brauher et al. 2008; Gracia-Carpio et al. 2011).”
Big Three Dragons: A z = 7.15 Lyman-break galaxy detected in [O iii] 88 μm, [C ii] 158 μm, and dust continuum with ALMA (2018, background): “A most commonly used line is [Cii] 158 µm, which is one of the brightest lines in local galaxies (e.g., Malhotra et al. 1997; Brauher et al. 2008).”
Detection of the Far-infrared [O iii] and Dust Emission in a Galaxy at Redshift 8.312: Early Metal Enrichment in the Heart of the Reionization Era (2018, methodology): “…simulation of galaxy formation (Shimizu et al. 2014) by incorporating an [O III] emission line model as a function of metallicity calibrated by ISO, AKARI, and Herschel observations of local galaxies (Brauher et al. 2008; Kawada et al. 2011; Madden et al. 2012, 2013, see also Cormier et al. 2015).”
The applicability of far-infrared fine-structure lines as star formation rate tracers over wide ranges of metallicities and galaxy types (2014, methodology): “(1) Brauher et al. (2008); (2) Graciá-Carpio et al. (in prep.)”
The Herschel Dwarf Galaxy Survey - I. Properties of the low-metallicity ISM from PACS spectroscopy (2015, methodology): “In this paper, the dwarf galaxy sample is primarily compared to the ISO LWS extragalactic sample of FIR fine-structure lines from Brauher et al. (2008) (hereafter B08), which is one of the most complete in the literature.”
OBSERVATIONS OF Arp 220 USING HERSCHEL-SPIRE: AN UNPRECEDENTED VIEW OF THE MOLECULAR GAS IN AN EXTREME STAR FORMATION ENVIRONMENT (2011, methodology): “Figure 3 shows the highest likelihood model fit to the SPIREFTS (blue - open circles), SPIRE-photometer (red - open triangles; listed in Table 2) and ISOLWS (red - open squares) data.”
A Herschel/PACS Far-infrared Line Emission Survey of Local Luminous Infrared Galaxies (2017, background): “…of the trends than a power-law fit, as it is known that the line to FIR ratios do not increase indefinitely at the lower end of the Tdust distribution and IR luminosities (e.g., Malhotra et al. 1997, 2001; Brauher et al. 2008; De Looze et al. 2014; Cormier et al. 2015; Herrera-Camus et al. 2015).”
Very extended cold gas, star formation and outflows in the halo of a bright QSO at z>6 (2014, background): “In local galaxies, early infrared space observatory (ISO) observations and, more recently, Herschel observations, have established a clear trend for decreasing [C ii]-to-FIR ratio with increasing FIR luminosity (Luhman et al. 2003; Brauher et al. 2008; Díaz-Santos et al. 2013).”