An Overview of the Dwarf Galaxy Survey

Madden, S.; Rémy-Ruyer, A.; Galametz, M.; Cormier, D.; Lebouteiller, V.; Galliano, F.; Hony, S.; Bendo, G. J.; Smith, M. W. L.; Pohlen, M.; Roussel, H.; Sauvage, M.; Wu, R.; Sturm, E.; Poglitsch, A.; Contursi, A.; Doublier, V.; Baes, M.; Barlow, M. J.; Boselli, A.; Boquien, M.; Carlson, L. R.; Ciesla, L.; Cooray, Asantha; Cortese, Luca; Looze, I. De; Irwin, Judith A.; Isaak, K. G.; Kamenetzky, J.; Karczewski, O. Ł.; Lu, N.; MacHattie, Jeremy A.; O’Halloran, B.; Parkin, T. J.; Rangwala, Naseem; Schirm, M. R. P.; Schulz, B.; Spinoglio, L.; Vaccari, M.; Wilson, C. D.; Wozniak, H.

doi:10.1086/671138

Cited by 214 publications

(150 citation statements)

References 216 publications

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“…More specifically, studies of optical and UV luminosity functions found that dwarf galaxies can contribute significantly to the faint end of the luminosity function (e.g., Liu et al 2008;Alavi et al 2016). Madden et al (2013), using Herschel, provides a rich far-IR and submm photometric and spectroscopic database for local dwarf galaxies covering a large range in metallicity (Dwarf Galaxy Survey-DGS). Focusing on the Herschel PACS spectroscopic data of the DGS, Cormier et al (2015) found an increasing trend of [C II] luminosity with increased metallicity among the dwarfs, where they cover a large range of [C II] luminosites (10 4-9 L e ) and metallicities (1/50-1 Z e ).…”

Section: Resultsmentioning

confidence: 99%

“…A better agreement between the two can be achieved if a CO-dependent ratio of log ([C II]/CO) is applied to the CO luminosity function where galaxies with higher CO luminosity have lower [C II]/CO ratio compared to those with lower CO luminosity. Theoretically this might be explained by CO being photodissociated into C and C + in low dust and metallicity environments by a strong far-UV field from young stars (e.g., Wolfire et al 2010;Madden et al 2013).…”

Section: Resultsmentioning

confidence: 99%

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THE LOCAL [C ii] 158 μm EMISSION LINE LUMINOSITY FUNCTION

Hemmati

Yan

Díaz-Santos

et al. 2016

ApJ

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We present, for the first time, the local [C II] 158 μm emission line luminosity function measured using a sample of more than 500 galaxies from the Revised Bright Galaxy Sample. [C II] luminosities are measured from the Herschel PACS observations of the Luminous Infrared Galaxies (LIRGs) in the Great Observatories All-sky LIRG Survey and estimated for the rest of the sample based on the far-infrared (far-IR) luminosity and color. The sample covers 91.3% of the sky and is complete at S 60 μm >5.24 Jy. We calculate the completeness as a function of [C II] line luminosity and distance, based on the far-IR color and flux densities. The [C II] luminosity function is constrained in the range ∼10 7-9 L e from both the 1/V max and a maximum likelihood methods. The shape of our derived [C II] emission line luminosity function agrees well with the IR luminosity function. For the CO(1-0) and [C II] luminosity functions to agree, we propose a varying ratio of [C II]/CO(1-0) as a function of CO luminosity, with larger ratios for fainter CO luminosities. Limited [C II] high-redshift observations as well as estimates based on the IR and UV luminosity functions are suggestive of an evolution in the [C II] luminosity function similar to the evolution trend of the cosmic star formation rate density. Deep surveys using the Atacama Large Millimeter Array with full capability will be able to confirm this prediction.

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Section: Resultsmentioning

confidence: 99%

Section: Resultsmentioning

confidence: 99%

THE LOCAL [C ii] 158 μm EMISSION LINE LUMINOSITY FUNCTION

Hemmati

Yan

Díaz-Santos

et al. 2016

ApJ

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“…In the following, we consider local galaxies from the KINGFISH sample (Kennicutt et al 2011), the GOALS sample (Sanders et al 2003;Armus et al 2009), and the Dwarf Galaxy Survey (DGS; Madden et al 2013). Combining these samples allows us to cover a wide range in galaxy properties.…”

Section: The Sample Of Herschel Observed Local Galaxiesmentioning

confidence: 99%

Are High-redshift Galaxies Hot? Temperature of z > 5 Galaxies and Implications for Their Dust Properties

Faisst

Capak

Yan

et al. 2017

ApJ

127

163

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Recent studies have found a significant evolution and scatter in the relationship between the UV spectral slope (β UV ) and the infrared excess (IRX; L IR /L UV ) at z>4, suggesting different dust properties of these galaxies. The total farinfrared (FIR) luminosity is key for this analysis, but it is poorly constrained in normal (main-sequence) star-forming z>5 galaxies, where often only one single FIR point is available. To better inform estimates of the FIR luminosity, we construct a sample of local galaxies and three low-redshift analogues of z>5 systems. The trends in this sample suggest that normal high-redshift galaxies have a warmer infrared (IR) spectral energy distribution (SED) compared to average z<4 galaxies that are used as priors in these studies. The blueshifted peak and mid-IR excess emission could be explained by a combination of a larger fraction of metal-poor interstellar medium being optically thin to ultraviolet (UV) light and a stronger UV radiation field due to high star formation densities. Assuming a maximally warm IR SED suggests a 0.6 dex increase in total FIR luminosities, which removes some tension between the dust attenuation models and observations of the IRX−βrelation at z>5. Despite this, some galaxies still fall below the minimum IRX −βrelation derived with standard dust cloud models. We propose that radiation pressure in these highly star-forming galaxies causes a spatial offset between dust clouds and young star-forming regions within the lifetime of O/B stars. These offsets change the radiation balance and create viewing-angle effects that can change UV colors at fixed IRX. We provide a modified model that can explain the location of these galaxies on the IRX−βdiagram.

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“…The distribution of dust mass surface density is inferred from infrared data from the Herschel Dwarf Galaxy Survey (Madden et al 2013). We model the infrared spectral energy distribution (SED) between 70 and 500 μm using a modified blackbody, the Draine & Li (2007) model, and the Galliano et al (2011) model with an amorphous carbonaceous component (see Galametz et al 2010;Rémy-Ruyer et al 2015 for details).…”

Section: Atomic Gas and Dustmentioning

confidence: 99%

Physical Properties of Molecular Clouds at 2 pc Resolution in the Low-metallicity Dwarf Galaxy NGC 6822 and the Milky Way

Schruba

Leroy

Kruijssen

et al. 2017

ApJ

116

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We present the Atacama Large Millimeter/submillimeter Array survey of CO(2-1) emission from the 1/5 solar metallicity, Local Group dwarf galaxy NGC6822. We achieve high (  » 0. 9 2 pc) spatial resolution while covering a large area: four 250 pc × 250 pc regions that encompass~2 3 of NGC6822ʼs star formation. In these regions, we resolve~150 compact CO clumps that have small radii (∼2-3 pc), narrow line width (~1 km s −1 ), and low filling factor across the galaxy. This is consistent with other recent studies of low-metallicity galaxies, but here shown with a15 larger sample. At parsec scales, CO emission correlates with m 8 m emission better than with m 24 m emission and anticorrelates with Hα, so that polycyclic aromatic hydrocarbon emission may be an effective tracer of molecular gas at low metallicity. The properties of the CO clumps resemble those of similar-size structures in Galactic clouds except of slightly lower surface brightness and with CO-to-H 2 ratio ∼1-2× the Galactic value. The clumps exist inside larger atomic-molecular complexes with masses typical for giant molecular clouds. Using dust to trace H 2 for the entire complex, we find the CO-to-H 2 ratio to be -20 25 the Galactic value, but with strong dependence on spatial scale and variations between complexes that may track their evolutionary state. The H 2 -to-H I ratio is low globally and only mildly above unity within the complexes. The ratio of star formation rate to H 2 is -3 5 higher in the complexes than in massive disk galaxies, but after accounting for the bias from targeting star-forming regions, we conclude that the global molecular gas depletion time may be as long as in massive disk galaxies.

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An Overview of the Dwarf Galaxy Survey

Cited by 214 publications

References 216 publications

THE LOCAL [C ii] 158 μm EMISSION LINE LUMINOSITY FUNCTION

THE LOCAL [C ii] 158 μm EMISSION LINE LUMINOSITY FUNCTION

Are High-redshift Galaxies Hot? Temperature of z > 5 Galaxies and Implications for Their Dust Properties

Physical Properties of Molecular Clouds at 2 pc Resolution in the Low-metallicity Dwarf Galaxy NGC 6822 and the Milky Way

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