THE<i>SPITZER</i>INFRARED NEARBY GALAXIES SURVEY: A HIGH-RESOLUTION SPECTROSCOPY ANTHOLOGY

Dale, Daniel A.; Smith, John David; Schlawin, Everett; Armus, L.; Buckalew, B.; Cohen, S.; Hélou, G.; Jarrett, T. H.; Johnson, L. Clifton; Moustakas, John; Murphy, E. J.; Roussel, H.; Sheth, Kartik; Staudaher, Shawn; Bot, Caroline; Calzetti, Daniela; Engelbracht, C. W.; Gordon, K. D.; Hollenbach, D. J.; Kennicutt, Robert C.; Malhotra, Sangeeta

doi:10.1088/0004-637x/693/2/1821

Cited by 77 publications

(131 citation statements)

References 82 publications

(101 reference statements)

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“…For the H  region properties of metal-rich galaxies, we refer to the studies on MIR ionic lines of the Spitzer Infrared Nearby Galaxies Survey (SINGS; Dale et al 2009) and of the luminous IR galaxies from GOALS (Inami et al 2013). We consider neon and sulphur measurements for the galaxies in the luminosity range L TIR 10 9 −10 12 L (∼190 sources (Giveon et al 2002;Verma et al 2003;Groves et al 2008).…”

Section: Line Ratios and Typical Conditions In Metal-rich Galaxiesmentioning

confidence: 99%

“…We consider neon and sulphur measurements for the galaxies in the luminosity range L TIR 10 9 −10 12 L (∼190 sources (Giveon et al 2002;Verma et al 2003;Groves et al 2008). A typical solution for the H  region of those metal-rich galaxies has an electron density n e 350 cm −3 and ionization parameter log U −3 (Dale et al 2009;Inami et al 2013). …”

Section: Line Ratios and Typical Conditions In Metal-rich Galaxiesmentioning

confidence: 99%

“…Median IRS line ratios with their dispersions in parenthesis, measured as 1.5 times the median absolute deviation in logarithmic space (Dale et al 2009 andInami et al 2013 for the metal-rich galaxies; this work for the low-metallicity, DGS galaxies). ISM abundances are taken from Cowie & Songaila (1986), Savage & Sembach (1996), Meyer et al (1998) is the effective radius of the H  region.…”

Section: Line Ratios and Typical Conditions In Metal-rich Galaxiesmentioning

confidence: 99%

“…The source of radiation is chosen as a young starburst that we simulate with Starburst99 (Leitherer et al 2010). Following Dale et al (2009), we adopt a 10 Myr continuous star formation scenario (with a Kroupa IMF and Geneva stellar tracks), and fix its luminosity to 10 9 L . We vary the following physical conditions: the hydrogen density (n H ; from 10 1.0 to 10 5.0 cm −3 in increments of 0.5 dex) and the inner radius (r in ; from 10 19.7 to 10 22.0 cm, or 15 pc to 3200 pc, in increments of 0.3 dex), which is the distance between the starburst and the surface of the modeled ISM shell.…”

Section: Model Parametersmentioning

confidence: 99%

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TheHerschelDwarf Galaxy Survey

Cormier

Madden

Lebouteiller

et al. 2015

A&A

234

399

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Context. The far-infrared (FIR) lines are important tracers of the cooling and physical conditions of the interstellar medium (ISM) and are rapidly becoming workhorse diagnostics for galaxies throughout the universe. There are clear indications of a different behavior of these lines at low metallicity that needs to be explored. Aims. Our goal is to explain the main differences and trends observed in the FIR line emission of dwarf galaxies compared to more metal-rich galaxies, and how this translates in ISM properties. ] 57 µm fine-structure cooling lines in a sample of 48 low-metallicity star-forming galaxies of the guaranteed time key program Dwarf Galaxy Survey. We correlate PACS line ratios and line-to-L TIR ratios with L TIR , L TIR /L B , metallicity, and FIR color, and interpret the observed trends in terms of ISM conditions and phase filling factors with Cloudy radiative transfer models. Results. We find that the FIR lines together account for up to 3 percent of L TIR and that star-forming regions dominate the overall emission in dwarf galaxies. Compared to metal-rich galaxies, the ratios of Harboring compact phases of a low filling factor and a large volume filling factor of diffuse gas, the ISM of low-metallicity dwarf galaxies has a more porous structure than that of metal-rich galaxies. Methods

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Section: Line Ratios and Typical Conditions In Metal-rich Galaxiesmentioning

confidence: 99%

Section: Line Ratios and Typical Conditions In Metal-rich Galaxiesmentioning

confidence: 99%

Section: Line Ratios and Typical Conditions In Metal-rich Galaxiesmentioning

confidence: 99%

Section: Model Parametersmentioning

confidence: 99%

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TheHerschelDwarf Galaxy Survey

Cormier

Madden

Lebouteiller

et al. 2015

A&A

234

399

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“…MIR diagnostic diagrams were presented by Sturm et al (2006), and Dale et al (2006Dale et al ( , 2009 to study ISM excitation mechanisms. Sturm et al (2006) compared the MIR properties (SED, PAHs, and emission line ratios) of IR-luminous and IRfaint LINERs.…”

Section: Introductionmentioning

confidence: 99%

Nearby early-type galaxies with ionized gas

Panuzzo

Rampazzo

Bressan

et al. 2011

A&A

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Context. A large fraction of early-type galaxies (ETGs) shows emission lines in their optical spectra, mostly with LINER characteristics. Despite the number of studies, the nature of the ionization mechanisms is still debated. Many ETGs also show several signs of rejuvenation episodes. Aims. We aim to investigate the ionization mechanisms and the physical processes of a sample of ETGs using mid-infrared spectra. Methods. We present here low resolution Spitzer-IRS spectra of 40 ETGs, 18 of which from our proposed Cycle 3 observations, selected from a sample of 65 ETGs showing emission lines in their optical spectra. We homogeneously extract the mid-infrared (MIR) spectra, and after the proper subtraction of a "passive" ETG template, we derive the intensity of the ionic and molecular lines and of the polycyclic aromatic hydrocarbon (PAH) emission features. We use MIR diagnostic diagrams to investigate the powering mechanisms of the ionized gas. Results. The mid-infrared spectra of early-type galaxies show a variety of spectral characteristics. We empirically sub-divide the sample into five classes of spectra with common characteristics. Class-0, accounting for 20% of the sample, are purely passive ETGs with neither emission lines nor PAH features. Class-1 show emission lines but no PAH features, and account for 17.5% of the sample. Class-2, in which 50% of the ETGs are found, as well as having emission lines, show PAH features with unusual ratios, e.g. 7.7 μm/11.3 μm ≤ 2.3. Class-3 objects (7.5% of the sample) have emission lines and PAH features with ratios typical of star-forming galaxies. Class-4, containing only 5% of the ETGs, is dominated by a hot dust continuum. .82 μm, is used to investigate the different mechanisms ionizing the gas. According to the above diagram most of our ETGs contain gas ionized via either AGN-like or shock phenomena, or both. Conclusions. Most of the spectra in the present sample are classified as LINERs in the optical window. The proposed MIR spectral classes show unambiguously the manifold of the physical processes and ionization mechanisms, from star formation, low level AGN activity, to shocks (H 2 ), present in LINER nuclei.

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2011

A Panchromatic View of Galaxies

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THESPITZERINFRARED NEARBY GALAXIES SURVEY: A HIGH-RESOLUTION SPECTROSCOPY ANTHOLOGY

Cited by 77 publications

References 82 publications

TheHerschelDwarf Galaxy Survey

TheHerschelDwarf Galaxy Survey

Nearby early-type galaxies with ionized gas

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