THE
 SPITZER
 SURVEY OF STELLAR STRUCTURE IN GALAXIES (S
 4
 G): PRECISE STELLAR MASS DISTRIBUTIONS FROM AUTOMATED DUST CORRECTION AT 3.6
 μ
 m

Querejeta, Miguel; Meidt, Sharon E.; Schinnerer, E.; Cisternas, Mauricio; Muñoz-Mateos, J. C.; Sheth, Kartik; Knapen, Johan H.; Ven, Glenn van de; Norris, Mark A.; Peletier, Reynier F.; Laurikainen, Eija; Salo, H.; Holwerda, Benne W.; Athanassoula, E.; Bosma, A.; Groves, Brent; Ho, Luis C.; Gadotti, Dimitri A.; Zaritsky, Dennis; Regan, Michael W.; Hinz, J. L.; Paz, A. Gil de; Menéndez‐Delmestre, Karín; Seibert, Mark; Mizusawa, Trisha; Kim, Tae Hyun; Erroz-Ferrer, Santiago; Laine, Jarkko; Comerón, Sébastien

doi:10.1088/0067-0049/219/1/5

Cited by 202 publications

(242 citation statements)

References 61 publications

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“…Our conclusion is that for the purpose of comparing the various profiles (dust, gas, stars) it is better to consider the IRAC images, weakly dependent on the dust with respect to the optical proxies, and the empirical relation of Querejeta et al (2015), that compares well with the results obtained with other methods in the literature and that is available for our entire sample.…”

Section: Stellar Masssupporting

confidence: 61%

“…They computed stellar mass maps using the Independent Component Analysis (ICA, Meidt et al 2012) which is able to disentangle the contribution of the light from old stars and the dust emission, that can significantly contribute to the observed 3.6 µm flux. Querejeta et al (2015) also provided a relationship between the effective stellar massto-light ratio (M/L) and the observed [3.6]-[4.5] color (with 0.2 dex of uncertainties), calibrated using their optimal stellar mass estimates and that compares well with other relations in the literature (e.g., Eskew et al 2012;Jarrett et al 2013;McGaugh & Schombert 2014).…”

Section: Stellar Massmentioning

confidence: 92%

“…The first method makes use of the MIR images, specifically the IRAC 3.6 and 4.5 µm, and the prescription presented in Querejeta et al (2015). They computed stellar mass maps using the Independent Component Analysis (ICA, Meidt et al 2012) which is able to disentangle the contribution of the light from old stars and the dust emission, that can significantly contribute to the observed 3.6 µm flux.…”

Section: Stellar Massmentioning

confidence: 99%

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Radial distribution of dust, stars, gas, and star-formation rate in DustPedia face-on galaxies

Casasola

Cassarà

Bianchi

et al. 2017

A&A

125

138

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Aims. The purpose of this work is the characterization of the radial distribution of dust, stars, gas, and star-formation rate (SFR) in a sub-sample of 18 face-on spiral galaxies extracted from the DustPedia sample. Methods. This study is performed by exploiting the multi-wavelength, from ultraviolet (UV) to sub-millimeter bands, DustPedia database, in addition to molecular ( 12 CO) and atomic (Hi) gas maps and metallicity abundance information available in the literature. We fitted the surface brightness profiles of the tracers of dust and stars, the mass surface density profiles of dust, stars, molecular gas, and total gas, and the SFR surface density profiles with an exponential curve and derived their scale-lengths. We also developed a method to solve for the CO-to-H 2 conversion factor (α CO ) per galaxy by using dust and gas mass profiles. Results. Although each galaxy has its own peculiar behaviour, we identified a common trend of the exponential scale-lengths vs. wavelength. On average, the scale-lengths normalized to the B-band 25 mag/arcsec 2 radius decrease from UV to 70 µm, from 0.4 to 0.2, and then increase back up to ∼0.3 at 500 microns. The main result is that, on average, the dust mass surface density scale-length is about 1.8 times the stellar one derived from IRAC data and the 3.6 µm surface brightness, and close to that in the UV. We found a mild dependence of the scale-lengths on the Hubble stage T: the scale-lengths of the Herschel bands and the 3.6 µm scale-length tend to increase from earlier to later types, the scale-length at 70 µm tends to be smaller than that at longer sub-mm wavelength with ratios between longer sub-mm wavelengths and 70 µm that decrease with increasing T. The scale-length ratio of SFR and stars shows a weak increasing trend towards later types. Our α CO determinations are in the range (0.3 − 9) M pc −2 (K km s −1 ) −1 , almost invariant by using a fixed dust-to-gas ratio mass (DGR) or a DGR depending on metallicity gradient.

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Section: Stellar Masssupporting

confidence: 61%

Section: Stellar Massmentioning

confidence: 92%

Section: Stellar Massmentioning

confidence: 99%

See 1 more Smart Citation

Radial distribution of dust, stars, gas, and star-formation rate in DustPedia face-on galaxies

Casasola

Cassarà

Bianchi

et al. 2017

A&A

125

138

View full text Add to dashboard Cite

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“…11 Using an enhanced correction for dust emission in the Spitzer/IRAC 3.6 μm image from the S 4 G pipeline 5 (Querejeta et al 2015), and considering information from beyond the edge of the PAWS FOV, Querejeta et al (2016) move the co-rotation of the inner spiral pattern to r∼100″. This is also consistent with the kinematic decomposition of the line-of-sight velocity field traced by the cold ISM, as performed by Colombo et al (2014b).…”

Section: Molecular Gas and Star Formation Across A Spiral Arm In M51mentioning

confidence: 57%

The PdBI Arcsecond Whirlpool Survey (PAWS): The Role of Spiral Arms in Cloud and Star Formation

Schinnerer

Meidt

Colombo

et al. 2017

ApJ

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The process that leads to the formation of the bright star-forming sites observed along prominent spiral arms remains elusive. We present results of a multi-wavelength study of a spiral arm segment in the nearby grand-design spiral galaxy M51 that belongs to a spiral density wave and exhibits nine gas spurs. The combined observations of the (ionized, atomic, molecular, dusty) interstellar medium with star formation tracers (H II regions, young <10 Myr stellar clusters) suggest (1) no variation in giant molecular cloud (GMC) properties between arm and gas spurs, (2) gas spurs and extinction feathers arising from the same structure with a close spatial relation between gas spurs and ongoing/recent star formation (despite higher gas surface densities in the spiral arm), (3) no trend in star formation age either along the arm or along a spur, (4) evidence for strong star formation feedback in gas spurs, (5) tentative evidence for star formation triggered by stellar feedback for one spur, and (6) GMC associations being not special entities but the result of blending of gas arm/spur cross sections in lower resolution observations. We conclude that there is no evidence for a coherent star formation onset mechanism that can be solely associated with the presence of the spiral density wave. This suggests that other (more localized) mechanisms are important to delay star formation such that it occurs in spurs. The evidence of star formation proceeding over several million years within individual spurs implies that the mechanism that leads to star formation acts or is sustained over a longer timescale.

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“…We also use the THINGS Hi map from Walter et al (2008) and a map of stellar surface density estimated from Spitzer near-IR photometry by Meidt et al (2012);Querejeta et al (2015) using a 3.6µm mass-to-light ratio of ∼ 0.5M ⊙ /L ⊙ , so that Σ ⋆ M ⊙ pc −2 = 350 I 3.6,corr MJy sr −1 . The Herschel and Spitzer data are extremely high signal to noise, so that the dominant uncertainty is the calibration.…”

Section: Observationsmentioning

confidence: 99%

The Empire Survey: Systematic Variations in the Dense Gas Fraction and Star Formation Efficiency From Full-Disk Mapping of M51

Bigiel

Leroy

Jiménez-Donaire

et al. 2016

ApJL

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120

225

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We present the first results from the EMPIRE survey, an IRAM large program that is mapping tracers of high density molecular gas across the disks of nine nearby star-forming galaxies. Here, we present new maps of the 3-mm transitions of HCN, HCO + , and HNC across the whole disk of our pilot target, M51. As expected, dense gas correlates with tracers of recent star formation, filling the "luminosity gap" between Galactic cores and whole galaxies. In detail, we show that both the fraction of gas that is dense, f dense traced by HCN/CO, and the rate at which dense gas forms stars, SFE dense traced by IR/HCN , depend on environment in the galaxy. The sense of the dependence is that high surface density, high molecular gas fraction regions of the galaxy show high dense gas fractions and low dense gas star formation efficiencies. This agrees with recent results for individual pointings by Usero et al. (2015) but using unbiased whole-galaxy maps. It also agrees qualitatively with the behavior observed contrasting our own Solar Neighborhood with the central regions of the Milky Way. The sense of the trends can be explained if the dense gas fraction tracks interstellar pressure but star formation occurs only in regions of high density contrast.

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THE SPITZER SURVEY OF STELLAR STRUCTURE IN GALAXIES (S ⁴ G): PRECISE STELLAR MASS DISTRIBUTIONS FROM AUTOMATED DUST CORRECTION AT 3.6 μ m

Cited by 202 publications

References 61 publications

Radial distribution of dust, stars, gas, and star-formation rate in DustPedia face-on galaxies

Radial distribution of dust, stars, gas, and star-formation rate in DustPedia face-on galaxies

The PdBI Arcsecond Whirlpool Survey (PAWS): The Role of Spiral Arms in Cloud and Star Formation

The Empire Survey: Systematic Variations in the Dense Gas Fraction and Star Formation Efficiency From Full-Disk Mapping of M51

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THE SPITZER SURVEY OF STELLAR STRUCTURE IN GALAXIES (S 4 G): PRECISE STELLAR MASS DISTRIBUTIONS FROM AUTOMATED DUST CORRECTION AT 3.6 μ m

Cited by 202 publications

References 61 publications

Radial distribution of dust, stars, gas, and star-formation rate in DustPedia face-on galaxies

Radial distribution of dust, stars, gas, and star-formation rate in DustPedia face-on galaxies

The PdBI Arcsecond Whirlpool Survey (PAWS): The Role of Spiral Arms in Cloud and Star Formation

The Empire Survey: Systematic Variations in the Dense Gas Fraction and Star Formation Efficiency From Full-Disk Mapping of M51

Contact Info

Product

Resources

About

THE SPITZER SURVEY OF STELLAR STRUCTURE IN GALAXIES (S ⁴ G): PRECISE STELLAR MASS DISTRIBUTIONS FROM AUTOMATED DUST CORRECTION AT 3.6 μ m