ALMACAL VIII: a pilot survey for untargeted extragalactic CO emission lines in deep ALMA calibration data

Hamanowicz, A.; Péroux, Céline; Lagos, Claudia del P.; Klitsch, Anne; Ivison, R. J.; Biggs, A. D.; Szakacs, Roland; Fresco, Alejandra

doi:10.1093/mnras/stac3159

Cited by 8 publications

(2 citation statements)

References 62 publications

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“…By detecting both low and medium to high-J transitions, it is also possible to study the redshift evolution of molecular gas in galaxies. Several studies have used ALMA and JVLA to perform blind line searches towards deep cosmological fields or ALMA calibrators (Walter et al 2016;González-López et al 2019;Riechers et al 2019Riechers et al , 2020Hamanowicz et al 2023). However, because of the large amount of telescope time needed, the surveyed area and the number of detected sources are still very limited.…”

Section: Introductionmentioning

confidence: 99%

Characterizing CO Emitters in SSA22-AzTEC26 Field

Huang¹,

Umehata²,

Kawabe³

et al. 2023

Preprint

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We report the physical characterization of four CO emitters detected near the bright submillimeter galaxy (SMG) SSA22-AzTEC26. We analyze the data from ALMA band 3, 4, and 7 observations of the SSA22-AzTEC26 field. In addition to the targeted SMG, we detect four line emitters with a signalto-noise ratio > 5.2 in the cube smoothed with 300 km s −1 FWHM Gaussian filter. All four sources have near-infrared (NIR) counterparts within 1 arcsec. We perform ultraviolet to far-infrared spectral energy distribution (SED) modeling to derive the photometric redshift and physical properties. Based on photometric redshifts, we reveal that two of them are CO(2-1) at redshifts of 1.113 and 1.146, and one is CO(3-2) at z = 2.124. The three sources are massive galaxies with a stellar mass 10 10.5 M , but have different levels of star formation. Two lie within the scatter of the main sequence (MS) of star-forming galaxies at z ∼ 1 − 2, and the most massive galaxy lies significantly below the MS. However, all three sources have a gas fraction within the scatter of the MS scaling relation. This shows that a blind CO line search can detect massive galaxies with low specific star formation rates that still host large gas reservoirs and complements targeted surveys, suggesting later gas acquisition and the need for other mechanisms in addition to gas consumption to suppress the star formation.

show abstract

Section: Introductionmentioning

confidence: 99%

Characterizing CO Emitters in SSA22-AzTEC26 Field

Huang¹,

Umehata²,

Kawabe³

et al. 2023

Preprint

View full text Add to dashboard Cite

show abstract

“…By detecting both low and medium to high J transitions, it is also possible to study the redshift evolution of the molecular gas in galaxies. Several studies have used the Atacama Large Millimeter/submillimeter Array and JVLA to perform blind line searches toward deep cosmological fields or ALMA calibrators (Walter et al 2016;González-López et al 2019;Riechers et al 2019Riechers et al , 2020Hamanowicz et al 2023). However, because of the large amounts of telescope time needed, the surveyed area and the number of detected sources are still very limited.…”

Section: Introductionmentioning

confidence: 99%

Characterizing CO Emitters in the SSA22-AzTEC26 Field

Huang

Umehata

Kawabe

et al. 2023

ApJ

View full text Add to dashboard Cite

We report the physical characterization of four CO emitters detected near the bright submillimeter galaxy (SMG) SSA22-AzTEC26. We analyze the data from Atacama Large Millimeter/submillimeter Array band 3, 4, and 7 observations of the SSA22-AzTEC26 field. In addition to the targeted SMG, we detect four line emitters with signal-to-noise ratio >5.2 in the cube smoothed with a 300 km s−1 FWHM Gaussian filter. All four sources have NIR counterparts within 1″. We perform UV-to-FIR spectral energy distribution modeling to derive the photometric redshifts and physical properties. Based on the photometric redshifts, we reveal that two of them are CO(2–1) at redshifts of 1.113 and 1.146 and one is CO(3–2) at z = 2.124. The three sources are massive galaxies with a stellar mass ≳1010.5 M ⊙, but have different levels of star formation. Two lie within the scatter of the main sequence (MS) of star-forming galaxies at z ∼ 1–2, and the most massive galaxy lies significantly below the MS. However, all three sources have a gas fraction within the scatter of the MS scaling relation. This shows that a blind CO line search can detect massive galaxies with low specific star formation rates that still host large gas reservoirs and that it also complements targeted surveys, suggesting later gas acquisition and the need for other mechanisms in addition to gas consumption to suppress star formation.

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Cold molecules in H I 21 cm absorbers across redshifts ∼0.1–4

Combes,

Gupta

2024

A&A

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Absorption lines at high redshift in front of quasars are quite rare in the millimeter (mm) domain. Only five associated and five intervening systems have been reported in the literature. Nevertheless, these discoveries provide very useful information that is complementary to emission lines, allowing, for instance, to distinguish between inflows and outflows. These lines are also good candidates for studying the variations of the fundamental constants of physics. Here we report the findings of our search for CO and other molecules in emission and absorption in front of a sample of 30 targets, comprising 16 associated and 14 intervening 21cm absorbers. The observations were made with the IRAM-30m telescope simultaneously at 3mm and 2mm, exploring several lines of the CO ladder and HCO$^+$, depending on the redshift. We detected eight targets in emission, of which five are new. The derived molecular gas masses range from 10$^9$ to 7times 1011 M$_ and the highest redshift detection ($z$ = 3.387) corresponds to a relatively average-metallicity damped Lyman-alpha absorber for this redshift. We also report four new detections in absorption. Two of the associated CO absorption line detections at high redshift ($z$=1.211 and 1.275) result from high-spatial-resolution follow-up observations with NOEMA. The disparity between the mm molecular and 21cm absorption lines for these and another intervening system detected in HNC at $z=1.275$ is attributable to radio and mm sight lines tracing different media. We compare the atomic and molecular column densities of 14 known high-redshift ($z$ > 0.1) molecular absorption line systems. The associated absorption lines are broad and exhibit multiple components, and the molecular absorption generally corresponds to the broader and weaker 21cm absorption component. This indicates two distinct phases: one near galaxy centers with a larger CO-to- abundance ratio, and another with lower molecular abundance in the outer regions of the galaxy. In comparison, intervening absorption profiles correspond primarily to gas structure in galaxy outskirts, except for gas at low impact parameters in gravitationally lensed systems. The comparison of interferometric and single-dish observations presented here shows that the detection of absorption requires sufficient spatial resolution to overcome the dilution by emission and will be an important criterion for mm follow-up of 21cm absorbers from ongoing large-scale surveys.

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ALMACAL VIII: a pilot survey for untargeted extragalactic CO emission lines in deep ALMA calibration data

Cited by 8 publications

References 62 publications

Characterizing CO Emitters in SSA22-AzTEC26 Field

Characterizing CO Emitters in SSA22-AzTEC26 Field

Characterizing CO Emitters in the SSA22-AzTEC26 Field

Cold molecules in H I 21 cm absorbers across redshifts ∼0.1–4

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ALMACAL VIII: a pilot survey for untargeted extragalactic CO emission lines in deep ALMA calibration data

Cited by 8 publications

References 62 publications

Characterizing CO Emitters in SSA22-AzTEC26 Field

Characterizing CO Emitters in SSA22-AzTEC26 Field

Characterizing CO Emitters in the SSA22-AzTEC26 Field

Cold molecules in H I 21 cm absorbers across redshifts ∼0.1–4

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Product

Resources

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Cold molecules in H I 21 cm absorbers across redshifts ∼0.1–4