“Super-deblended” Dust Emission in Galaxies. II. Far-IR to (Sub)millimeter Photometry and High-redshift Galaxy Candidates in the Full COSMOS Field

Jin, S.; Daddi, E.; Liu, Daizhong; Smolčić, Vernesa; Schinnerer, E.; Calabró, Antonello; Gu, Qiusheng; Delhaize, J.; Delvecchio, I.; Gao, Yu; Salvato, M.; Puglisi, A.; Dickinson, Mark; Bertoldi, F.; Sargent, M.; Novak, Mladen; Magdis, G.; Aretxaga, I.; Wilson, Grant; Capak, P.

doi:10.3847/1538-4357/aad4af

Cited by 158 publications

(272 citation statements)

References 107 publications

(181 reference statements)

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“…To extend the redshift range, we also utilize the latest COSMOS master spectroscopic catalog (curated by M. Salvato for internal use within the COSMOS collaboration), together with the COSMOS2015 (Laigle et al 2016) and "Super-deblended" (Jin et al 2018) photometric catalogs. The COSMOS2015 catalog provides photometry for the UV through NIR wavelength range from GALEX, CFHT, Subaru, UltraVista, and Spitzer /IRAC.…”

Section: Cosmos2015 and Super-deblended Samplementioning

confidence: 99%

The Strength of the 2175 Å Feature in the Attenuation Curves of Galaxies at 0.1 < z ≲ 3

Battisti

Cunha

Shivaei

et al. 2020

ApJ

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We update the spectral modeling code MAGPHYS to include a 2175Å absorption feature in its UV-tonear-IR dust attenuation prescription. This allows us to determine the strength of this feature and the shape of the dust attenuation curve in ∼5000 star-forming galaxies at 0.1 < z 3 in the COSMOS field. We find that a 2175Å absorption feature of ∼1/3 the strength of that in the Milky Way is required for models to minimize residuals. We characterize the total effective dust attenuation curves as a function of several galaxy properties and find that the UV slopes of the attenuation curve for COSMOS galaxies show a strong dependence with star formation rate (SFR) and total dust attenuation (A V ), such that galaxies with higher SFR and A V have shallower curves and vice versa. These results are consistent with expectations from radiative transfer that attenuation curves become shallower as the effective dust optical depth increases. We do not find significant trends in the strength of the 2175Å absorption feature as a function of galaxy properties, but this may result from the high uncertainties associated with this measurement. The updated code is publicly available online.Corresponding author: A. J. Battisti andrew.battisti@anu.edu.au 1 We define attenuation to be a combination of extinction, scattering of light into the line of sight by dust, and geometrical effects due to the star-dust geometry. Extinction is the absorption and scattering of light out of the line of sight by dust, which has no dependence on geometry. Unlike extinction curves, the geometric effects in attenuation make it difficult to interpret the physical properties of dust from attenuation curves.

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Section: Cosmos2015 and Super-deblended Samplementioning

confidence: 99%

The Strength of the 2175 Å Feature in the Attenuation Curves of Galaxies at 0.1 < z ≲ 3

Battisti

Cunha

Shivaei

et al. 2020

ApJ

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“…We fitted the rich multi-wavelength photometry in order to obtain physical information such as star formation Jin et al (2018), in which the emission in the FIR bands for each object is accurately deblended over multiple objects by using the position of the emission at shorter wavelength as a prior, in combination with UV-optical-NIR photometry from Laigle et al (2016). By checking the multiwavelength images, we realized that the photometry for one object, Gal2, is perturbed by a lower redshift interloper that is not deblended in the Laigle et al (2016) catalog: in fact, this interloper is detected in the U-band image, a band that at z∼3 would match the Lymancontinuum.…”

Section: Ancillary Data and Sed Fittingmentioning

confidence: 99%

ALMA Reveals the Molecular Gas Properties of Five Star-forming Galaxies across the Main Sequence at 3

Cassata

Liu

Groves

et al. 2020

ApJ

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We present the detection of CO(5-4) with S/N> 7 − 13 and a lower CO transition with S/N> 3 (CO(4-3) for 4 galaxies, and CO(3-2) for one) with ALMA in band 3 and 4 in five main sequence star-forming galaxies with stellar masses 3 − 6 × 10 10 M/M at 3 < z < 3.5. We find a good correlation between the total far-infrared luminosity L F IR and the luminosity of the CO(5-4) transition L CO(5−4) , where L CO(5−4) increases with SFR, indicating that CO(5-4) is a good tracer of the obscured SFR in these galaxies. The two galaxies that lie closer to the star-forming main sequence have CO SLED slopes that are comparable to other star-forming populations, such as local SMGs and BzK star-forming galaxies; the three objects with higher specific star formation rates (sSFR) have far steeper CO SLEDs, which possibly indicates a more concentrated episode of star formation. By exploiting the CO SLED slopes to extrapolate the luminosity of the CO(1-0) transition, and using a classical conversion factor for main sequence galaxies of α CO = 3.8 M (K km s −1 pc −2 ) −1 , we find that these galaxies are very gas rich, with molecular gas fractions between 60 and 80%, and quite long depletion times, between 0.2 and 1 Gyr. Finally, we obtain dynamical masses that are comparable with the sum of stellar and gas mass (at least for four out of five galaxies), allowing us to put a first constraint on the α CO parameter for main sequence galaxies at an unprecedented redshift.

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“…The sample used is described in detail in Laigle et al (2016), which provides robust multi-wavelength restframe magnitudes. Galaxies are then cross-matched with a FIR/mm catalog (Sanders et al 2007;Jin et al 2018) over the same footprint. Objects with MIPS SNR < 3 are considered too faint for a MIPS nondetection to be a reliable indicator of quiescence, and are not included in the sample.…”

Section: Comparison With Template Fittingmentioning

confidence: 99%

A Method to Distinguish Quiescent and Dusty Star-forming Galaxies with Machine Learning

Steinhardt¹,

Weaver²,

Maxfield

et al. 2020

ApJ

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Large photometric surveys provide a rich source of observations of quiescent galaxies, including a surprisingly large population at z > 1. However, identifying large, but clean, samples of quiescent galaxies has proven difficult because of their near-degeneracy with interlopers such as dusty, starforming galaxies. We describe a new technique for selecting quiescent galaxies based upon t-distributed stochastic neighbor embedding (t-SNE), an unsupervised machine learning algorithm for dimensionality reduction. This t-SNE selection provides an improvement both over UVJ, removing interlopers which otherwise would pass color selection, and over photometric template fitting, more strongly towards high redshift. Due to the similarity between the colors of high-and low-redshift quiescent galaxies, under our assumptions t-SNE outperforms template fitting in 63% of trials at redshifts where a large training sample already exists. It also may be able to select quiescent galaxies more efficiently at higher redshifts than the training sample.

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“Super-deblended” Dust Emission in Galaxies. II. Far-IR to (Sub)millimeter Photometry and High-redshift Galaxy Candidates in the Full COSMOS Field

Cited by 158 publications

References 107 publications

The Strength of the 2175 Å Feature in the Attenuation Curves of Galaxies at 0.1 < z ≲ 3

The Strength of the 2175 Å Feature in the Attenuation Curves of Galaxies at 0.1 < z ≲ 3

ALMA Reveals the Molecular Gas Properties of Five Star-forming Galaxies across the Main Sequence at 3

A Method to Distinguish Quiescent and Dusty Star-forming Galaxies with Machine Learning

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