A high dust emissivity index β for a CO-faint galaxy in a filamentary Lyα nebula at <i>z</i> = 3.1

Kato, Yuta; Matsuda, Yoshihisa; Iono, Daisuke; Hatsukade, Bunyo; Umehata, Hideki; Kohno, Kotaro; Alexander, D. M.; Ao, Yiping; Chapman, Scott; Hayes, Matthew; Kubo, Mariko; Lehmer, Bret; Malkan, Matthew A.; Michiyama, Tomonari; Nagao, Tohru; Saito, Tomoki; Tanaka, Ichi; Taniguchi, Yoshiaki

doi:10.1093/pasj/psy087

Cited by 12 publications

(10 citation statements)

References 63 publications

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“…This might be in line with recent results reporting steeper values in > 3 galaxies (e.g. Kato et al 2018;Jin et al 2019;Casey et al in prep. ), suggesting an evolution of the dust emissivity index with redshift and/or luminosity.…”

Section: On the Nature Of Non-detectionssupporting

confidence: 92%

Early science with the Large Millimeter Telescope: a 1.1 mm AzTEC survey of red-Herschel dusty star-forming galaxies

Montaña

Zavala

Aretxaga

et al. 2021

Monthly Notices of the Royal Astronomical Society

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We present LMT/AzTEC 1.1mm observations of ∼100 luminous high-redshift dusty star-forming galaxy candidates from the ∼600 sq.deg Herschel-ATLAS survey, selected on the basis of their SPIRE red far-infrared colours and with $S_{500\, \mu \rm m}=35-80$ mJy. With an effective θFWHM ≈ 9.5 arcsec angular resolution, our observations reveal that at least 9 per cent of the targets break into multiple systems with SNR ≥4 members. The fraction of multiple systems increases to ∼23 per cent (or more) if some non-detected targets are considered multiples, as suggested by the data. Combining the new AzTEC and deblended Herschel photometry we derive photometric redshifts, IR luminosities, and star formation rates. While the median redshifts of the multiple and single systems are similar (zmed ≈ 3.6), the redshift distribution of the latter is skewed towards higher redshifts. Of the AzTEC sources ∼85 per cent lie at zphot > 3 while ∼33 per cent are at zphot > 4. This corresponds to a lower limit on the space density of ultra-red sources at 4 < z < 6 of ∼3 × 10−7 Mpc−3 with a contribution to the obscured star-formation of ≳ 8 × 10−4 M⊙ yr−1 Mpc−3. Some of the multiple systems have members with photometric redshifts consistent among them suggesting possible physical associations. Given their angular separations, these systems are most likely galaxy over-densities and/or early-stage pre-coalescence mergers. Finally, we present 3mm LMT/RSR spectroscopic redshifts of six red-Herschel galaxies at zspec = 3.85 − 6.03, two of them (at z ∼ 4.7) representing new redshift confirmations. Here we release the AzTEC and deblended Herschel photometry as well as catalogues of the most promising interacting systems and z > 4 galaxies.

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Section: On the Nature Of Non-detectionssupporting

confidence: 92%

Early science with the Large Millimeter Telescope: a 1.1 mm AzTEC survey of red-Herschel dusty star-forming galaxies

Montaña

Zavala

Aretxaga

et al. 2021

Monthly Notices of the Royal Astronomical Society

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“…With our sample we not only confirm this value to be a reasonable average value for highredshift dusty star-forming galaxies (β ; 1.5-2 is often assumed when modeling sources at both low and high redshift; e.g., Scoville et al 2016;Galliano et al 2018) but also show that there can be significant variation from galaxy to galaxy. We note that the recent ALMA measurement of β = 2.3 in a z = 3.1 galaxy by Kato et al (2018) is entirely consistent with the range of values we find for our SMGs, and therefore that source is not necessarily an outlier in dust properties. The recent sample of 47 SMGs from Birkin et al (2021) yields β = 2.1 ± 0.1, consistent with our results (J. Birkin, private communication).…”

Section: Comparison With Other Measurements and Theoretical Predictionssupporting

confidence: 91%

Measurements of the Dust Properties in z ≃ 1–3 Submillimeter Galaxies with ALMA

Cunha

Hodge

Casey

et al. 2021

ApJ

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We present Atacama Large Millimeter/submillimeter Array (ALMA) 2 mm continuum observations of a complete and unbiased sample of 99 870 μm selected submillimeter galaxies (SMGs) in the Extended Chandra Deep Field South (ALESS). Our observations of each SMG reach average sensitivities of 53 μJy beam −1 . We measure the flux densities for 70 sources, for which we obtain a typical 870 μm-to-2 mm flux ratio of 14 ± 5. We do not find a redshift dependence of this flux ratio, which would be expected if the dust emission properties of our SMGs were the same at all redshifts. By combining our ALMA measurements with existing Herschel/SPIRE observations, we construct a (biased) subset of 27 galaxies for which the cool dust emission is sufficiently well sampled to obtain precise constraints on their dust properties using simple isothermal models. Thanks to our new 2 mm observations, the dust emissivity index is well constrained and robust against different dust opacity assumptions. The median dust emissivity index of our SMGs is β ; 1.9 ± 0.4, consistent with the emissivity index of dust in the Milky Way and other local and high-redshift galaxies, as well as classical dust-grain model predictions. We also find a negative correlation between the dust temperature and β, similar to low-redshift observational and theoretical studies. Our results indicate that β ; 2 in high-redshift dusty star-forming galaxies, implying little evolution in dust-grain properties between our SMGs and local dusty galaxy samples, and suggesting that these high-mass and highmetallicity galaxies have dust reservoirs driven by grain growth in their interstellar medium.

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“…We find β = 2.7 ± 0.4 and T = 7.2 ± 1.1, with χ 2 = 2.31 and 1 degree of freedom, the probability to exceed (χ 2 ) due to noise alone is 0.128. This value of β is higher than perhaps expected (Draine & Lee 1984), although β > 2 has been found (e.g Kato et al 2018), and even β > 3 have been found (e.g. references within Shetty et al 2009).…”

Section: C1 Pressure Profile Fitting and Resultsmentioning

confidence: 59%

“…references within Shetty et al 2009). As in Kato et al (2018), source blending may also affect our Herschel photometry.…”

mentioning

confidence: 98%

Pressure Profiles and Mass Estimates Using High-resolution Sunyaev–Zel’dovich Effect Observations of Zwicky 3146 with MUSTANG-2

Romero

Sievers

Ghirardini

et al. 2020

ApJ

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The galaxy cluster Zwicky 3146 is a sloshing cool core cluster at z = 0.291 that in X-ray imaging does not appear to exhibit significant pressure substructure in the intracluster medium (ICM). The published M 500 values range between 3.88 +0.62 −0.58 to 22.50 ± 7.58 × 10 14 M , where ICM-based estimates with reported errors < 20% suggest that we should expect to find a mass between 6.53 +0.44 −0.44 × 10 14 M (from Planck, with an 8.4σ detection) and 8.52 +1.77 −1.47 × 10 14 M (from ACT, with a 14σ detection). This broad range of masses is suggestive that there is ample room for improvement for all methods. Here, we investigate the ability to estimate the mass of Zwicky 3146 via the Sunyaev-Zel'dovich (SZ) effect with data taken at 90 GHz by MUSTANG-2 to a noise level better than 15 µK at the center, and a cluster detection of 104σ. We derive a pressure profile from our SZ data which is in excellent agreement with that derived from X-ray data. From our SZ-derived pressure profiles, we infer M 500 and M 2500 via three methods -Y -M scaling relations, the virial theorem, and hydrostatic equilibrium -where we employ X-ray constraints from XMM-Newton on the electron density profile when assuming hydrostatic equilibrium. Depending on the model and estimation method, our M 500 estimates range from 6.23 ± 0.59 to 10.6 ± 0.95 × 10 14 M , where our estimate from hydrostatic equilibrium, is 8.29 +1.93 −1.24 (±19.1% stat) +0.74 −0.68 (±8.6% sys, calibration) ×10 14 M . Our fiducial mass, derived from a Y -M relation is 8.16 +0.44 −0.54 (±5.5% stat) +0.46 −0.43 (±5.5% sys, Y -M ) +0.59 −0.55 (±7.0% sys, cal.) ×10 14 M . We investigate the consistency of our mass estimates and potential for otherwise unaddressed systematic errors within the MUSTANG-2 data. The inconsistencies among our mass estimates are not well explained by a potential systematic error in the MUSTANG-2 data.

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A high dust emissivity index β for a CO-faint galaxy in a filamentary Lyα nebula at z = 3.1

Abstract: We present CO J = 4 − 3 line and 3 mm dust continuum observations of a 100 kpcscale filamentary Lyα nebula (SSA22 LAB18) at z = 3.1 using the Atacama Large Millimeter/submillimeter Array (ALMA). We detected the CO J = 4 − 3 line at a systemic

Cited by 12 publications

References 63 publications

Early science with the Large Millimeter Telescope: a 1.1 mm AzTEC survey of red-Herschel dusty star-forming galaxies

Early science with the Large Millimeter Telescope: a 1.1 mm AzTEC survey of red-Herschel dusty star-forming galaxies

Measurements of the Dust Properties in z ≃ 1–3 Submillimeter Galaxies with ALMA

Pressure Profiles and Mass Estimates Using High-resolution Sunyaev–Zel’dovich Effect Observations of Zwicky 3146 with MUSTANG-2

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