The effects of star formation on the low-metallicity ISM: NGC 4214 mapped with<i>Herschel</i>/PACS spectroscopy

Cormier, D.; Madden, S.; Hony, S.; Contursi, A.; Poglitsch, A.; Galliano, F.; Sturm, E.; Doublier, V.; Feuchtgruber, H.; Galametz, M.; Geis, N.; Jong, Jeroen de; Okumura, K.; Panuzzo, P.; Sauvage, M.

doi:10.1051/0004-6361/201014699

Cited by 51 publications

(74 citation statements)

References 23 publications

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“…The luminosities reported by Cormier et al (2010) L and 2×10 6 L , respectively, which together represent 2.88% (4.26%) of the total luminosity measured in the PACS 160 (MIPS 160) band.…”

Section: Line Contaminationmentioning

confidence: 83%

“…We estimated the flux of the CO(2-1) line from the measured CO(1-0) value assuming that the line intensity ratio it is given by the value for optically thick, thermalized CO, I CO(1−0) /I CO(2−1) = 1. The contribution of the CO(2-1) line to Cormier et al (2010). With a field of view of 1.6 x 1.6 , only the central part of the galaxy is observed.…”

Section: Line Contaminationmentioning

confidence: 99%

“…An indication for this is e.g. the very high CII/CO ratio measured in the central region (Cormier et al 2010), which shows that a large fraction of the CO is photo-dissociated owing to the high radiation field and low dust shielding. Even though the X-factor has been notoriously difficult to determine, progress has been made in recent years mainly due to the possibility to derive dust masses with an increasingly better precision.…”

Section: Gas-to-dust Mass Ratiomentioning

confidence: 99%

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The dust SED of dwarf galaxies

Hermelo

Lisenfeld

Relaño

et al. 2012

A&A

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Context. High-resolution data from Spitzer, Herschel, and Planck allow us to probe the entire spectral energy distribution (SED) of morphologically separated components of the dust emission from nearby galaxies and allow a more detailed comparison between data and models. Aims. We wish to establish the physical origin of dust heating and emission based on radiation transfer models, that self-consistently connect the emission components from diffuse dust and the dust in massive star forming regions. Methods. NGC 4214 is a nearby dwarf galaxy with a large set of ancillary data, ranging from the ultraviolet (UV) to radio, including maps from Spitzer and Herschel and detections from Planck. We mapped this galaxy with MAMBO at 1.2 mm at the IRAM 30 m telescope. We extracted separate dust emission components for the HII regions (plus their associated PDRs on pc scales) and for the diffuse dust (on kpc scales). We analysed the full UV to FIR/submm SED of the galaxy using a radiation transfer model that self-consistently treats the dust emission from diffuse and star forming (SF) complexes components, considering the illumination of diffuse dust both by the distributed stellar populations and by escaping light from the HII regions. While maintaining consistency within the framework of this model, we additionally used a model that provides a detailed description of the dust emission from the HII regions and their surrounding PDRs on pc scales. Thanks to the large amount of available data and many previous studies for NGC 4214, very few free parameters remained in the model fitting process. Results. We achieve a satisfactory fit for the emission from HII + PDR regions on pc scales, with the exception of the emission at 8 μm, which is underpredicted by the model. For the diffuse emission we achieve a good fit if we assume that about 40-65% of the emission escaping the HII + PDR regions is able to leave the galaxy without passing through a diffuse ISM, which is not an unlikely scenario for a dwarf galaxy that has recently undergone a nuclear starburst. We determine a dust-to-gas mass ratio of 350-470, which is close to the expected value based on the metallicity.

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“…The luminosities reported by Cormier et al (2010) L and 2×10 6 L , respectively, which together represent 2.88% (4.26%) of the total luminosity measured in the PACS 160 (MIPS 160) band.…”

Section: Line Contaminationmentioning

confidence: 83%

Section: Line Contaminationmentioning

confidence: 99%

Section: Gas-to-dust Mass Ratiomentioning

confidence: 99%

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The dust SED of dwarf galaxies

Hermelo

Lisenfeld

Relaño

et al. 2012

A&A

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“…Stacey et al 1991, Cormier et al 2010. High may be boosted by the AGN and the metallicity hence overestimated.…”

Section: Normal [C Ii]/co Emissionmentioning

confidence: 99%

ALMA detection of [C ii] 158μm emission from a strongly lensedz= 2.013 star-forming galaxy

Schaerer

Boone

Jones

et al. 2015

A&A

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Aims. Our objectives are to determine the properties of the interstellar medium (ISM) and of star formation in typical star-forming galaxies at high redshift. Methods. Following up on our previous multi-wavelength observations with HST, Spitzer, Herschel, and the Plateau de Bure Interferometer (PdBI), we have studied a strongly lensed z = 2.013 galaxy, the arc behind the galaxy cluster MACS J0451+0006, with ALMA to measure the [C ] 158 µm emission line, one of the main coolants of the ISM. Results. Emission of the [C ] line from the southern part of this galaxy is detected at 10σ. Taking strong gravitational lensing into account, which provides a magnification of µ = 49, the intrinsic lensing-corrected, is found to be similar to that in nearby galaxies. The same also holds for the observed ratio L [CII] /L CO = 2.3 × 10 3 , which is comparable to that of star-forming galaxies and active galaxy nuclei (AGN) at low redshift. Conclusions. We utilize strong gravitational lensing to extend diagnostic studies of the cold ISM to an order of magnitude lower luminosity (L IR ∼ (1.1−1.3) × 10 11 L ) and SFR than previous work at high redshift. While larger samples are needed, our results provide evidence that the cold ISM of typical high-redshift galaxies has physical characteristics similar to normal star-forming galaxies in the local Universe.

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“…This [C] line is considered to be the dominant coolant for neutral atomic gas in the ISM (Tielens & Hollenbach 1985a,b;Wolfire et al 1995) and, therefore, among the brightest emission lines originating from star-forming galaxies (e.g., Stacey et al 1991;Malhotra et al 1997;Brauher et al 2008). In particular, low-metallicity galaxies show exceptionally strong [C] line emission (e.g., Poglitsch et al 1995;Madden et al 1997;Madden 2000;Hunter et al 2001;Cormier et al 2010;Israel & Maloney 2011). Carbon has an ionization potential of 11.3 eV (compared to 13.6 eV for hydrogen), implying that line emission can originate from neutral and ionized gas components (see Table 1).…”

Section: Introductionmentioning

confidence: 99%

The applicability of far-infrared fine-structure lines as star formation rate tracers over wide ranges of metallicities and galaxy types

Looze

Cormier

Lebouteiller

et al. 2014

A&A

403

382

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Aims. We analyze the applicability of far-infrared fine-structure lines [C] 158 µm, [O] 63 µm, and [O] 88 µm 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 µm) and farinfrared 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 [O] 63 and [O] 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 [C] 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 [C] and [O] 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 [O]

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The effects of star formation on the low-metallicity ISM: NGC 4214 mapped withHerschel/PACS spectroscopy

Cited by 51 publications

References 23 publications

The dust SED of dwarf galaxies

The dust SED of dwarf galaxies

ALMA detection of [C ii] 158μm emission from a strongly lensedz= 2.013 star-forming galaxy

The applicability of far-infrared fine-structure lines as star formation rate tracers over wide ranges of metallicities and galaxy types

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