Full of Orions: a 200-pc mapping of the interstellar medium in the redshift-3 lensed dusty star-forming galaxy SDP.81

Rybak, Matus; Hodge, J. A.; Vegetti, Simona; Werf, P. P. van der; Andreani, P.; Graziani, Luca; McKean, J. P.

doi:10.1093/mnras/staa879

Cited by 37 publications

(50 citation statements)

References 110 publications

(200 reference statements)

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“…The relatively compact size of the FIR continuum emission in FIR-bright sources also appears to hold with respect to the [CII] 158 μm emission (e.g. [ 310 , 329 , 426 , 459 , 460 ]), where the latter is now routinely detected (including serendipitously; e.g. [ 290 , 426 ]) and resolved with ALMA.…”

Section: Ism Properties Of Galaxies At Cosmic Noon and Beyondmentioning

confidence: 85%

“…A similar conclusion was reached by Gullberg et al [ 329 ] and Rybak et al [ 410 ], who used the capabilities of ALMA to extend such resolved studies to unlensed SMGs. Rybak et al [ 310 , 410 ] further argue that the slope of the deficit in the L

/L FIR -versus-Σ SFR plane is consistent with thermal saturation of the [CII] line at high gas temperatures. This explanation was proposed previously by Muñoz & Oh [ 471 ], but was not found to hold for the source studied by Litke et al [ 470 ].…”

Section: Ism Properties Of Galaxies At Cosmic Noon and Beyondmentioning

confidence: 87%

“…The low value derived for the Toomre stability parameter ( Q ∼ 0.3; [ 248 , 309 ]) suggests an unstable disc. Swinbank et al [ 309 ] compare the scaling relations observed between luminosity, line-widths and sizes, finding evidence for an offset from local molecular clouds that can be attributed to an external hydrostatic pressure for the interstellar medium that is approximately 10 4 × higher than the typical pressure in the Milky Way, and Rybak et al [ 310 ] use photon-dominated region (PDR) models to further constrain the physical conditions of the star-forming gas. The unprecedented SDP.81 data also allowed a study of dark matter substructure in the foreground lens halo itself [ 311 ], which is a separate topic beyond the scope of this review.…”

Section: Submillimetre-selected Galaxies Followed Up By Almamentioning

confidence: 99%

“…The importance of dust temperature gradients was also recognized by Cochrane et al [ 458 ], whose radiative transfer modelling of galaxies from the FIRE-2 simulations demonstrated that, due to dust heating, the spatial extent of the observed dust continuum emission is sensitive to the scale of recent star formation. On the other hand, the multi-band continuum imaging of the resolved z = 3 source SDP.81 shows no evidence for a varying dust temperature across the source [ 310 ]. Nevertheless, caution should be exercised when using the FIR continuum to trace the cool gas (§ 3.1.1 ) in a resolved sense without taking into account potential variations in dust temperature and gas column density.…”

Section: Ism Properties Of Galaxies At Cosmic Noon and Beyondmentioning

confidence: 99%

“…For instance, Popping et al [ 511 ] used ALMA observations of [CI](1–0), CO(3–2), CO(4–3) and the FIR continuum in a z = 2.2 ‘compact star-forming galaxy’ (cSFG) to put constraints on its gas density and UV radiation field strength, deriving starburst-like ISM properties despite its location on the ‘main sequence’. Meanwhile, Rybak et al [ 310 ] used the angular resolution provided by ALMA in multiple tracers in combination with strong lensing to map these parameters within the z = 3 source SDP.81 on approximately 200 pc scales.…”

Section: Ism Properties Of Galaxies At Cosmic Noon and Beyondmentioning

confidence: 99%

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High-redshift star formation in the Atacama large millimetre/submillimetre array era

2020

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The Atacama Large Millimetre/submillimetre Array (ALMA) is currently in the process of transforming our view of star-forming galaxies in the distant ( z ≳ 1 ) universe. Before ALMA, most of what we knew about dust-obscured star formation in distant galaxies was limited to the brightest submillimetre sources—the so-called submillimetre galaxies (SMGs)—and even the information on those sources was sparse, with resolved (i.e. sub-galactic) observations of the obscured star formation and gas reservoirs typically restricted to the most extreme and/or strongly lensed sources. Starting with the beginning of early science operations in 2011, the last 9 years of ALMA observations have ushered in a new era for studies of high-redshift star formation. With its long baselines, ALMA has allowed observations of distant dust-obscured star formation with angular resolutions comparable to—or even far surpassing—the best current optical telescopes. With its bandwidth and frequency coverage, it has provided an unprecedented look at the associated molecular and atomic gas in these distant galaxies through targeted follow-up and serendipitous detections/blind line scans. Finally, with its leap in sensitivity compared to previous (sub-)millimetre arrays, it has enabled the detection of these powerful dust/gas tracers much further down the luminosity function through both statistical studies of colour/mass-selected galaxy populations and dedicated deep fields. We review the main advances ALMA has helped bring about in our understanding of the dust and gas properties of high-redshift ( z ≳ 1 ) star-forming galaxies during these first 9 years of its science operations, and we highlight the interesting questions that may be answered by ALMA in the years to come.

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Section: Ism Properties Of Galaxies At Cosmic Noon and Beyondmentioning

confidence: 85%

Section: Ism Properties Of Galaxies At Cosmic Noon and Beyondmentioning

confidence: 87%

Section: Submillimetre-selected Galaxies Followed Up By Almamentioning

confidence: 99%

Section: Ism Properties Of Galaxies At Cosmic Noon and Beyondmentioning

confidence: 99%

Section: Ism Properties Of Galaxies At Cosmic Noon and Beyondmentioning

confidence: 99%

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High-redshift star formation in the Atacama large millimetre/submillimetre array era

2020

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[C II] 158 μm line emission from Orion A I. A template for extragalactic studies?

Pabst

Hacar

Goicoechea

et al. 2021

A&A

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Context. The [C II] 158 μm fine-structure line is one of the dominant coolants of the neutral interstellar medium. It is hence one of the brightest far-infrared (FIR) emission lines and can be observed not only in star-forming regions throughout the Galaxy, but also in the diffuse interstellar medium and in distant galaxies. [C II] line emission has been suggested to be a powerful tracer of star formation. Aims. We aim to understand the origin of [C II] emission and its relation to other tracers of interstellar gas and dust. This includes a study of the heating efficiency of interstellar gas as traced by the [C II] line to test models of gas heating. Methods. We made use of a one-square-degree map of velocity-resolved [C II] line emission toward the Orion Nebula complex, including M 43 and NGC 1977. We employed Herschel FIR photometric images to determine dust properties. Moreover, we compared with Hα emission from the ionized gas, Spitzer mid-infrared photometry to trace hot dust and large polycyclic aromatic hydrocarbons (PAHs), and velocity-resolved IRAM 30m CO(2–1) observations of the molecular gas. Results. The [C II] intensity is tightly correlated with PAH emission in the IRAC 8 μm band and FIR emission from warm dust. However, the [C II] intensity depends less than linearly on the 8 μm and FIR intensity, while 8 μm and FIR intensities are approximately linearly correlated. The correlation between [C II] and CO(2–1) does not show a clear trend and is affected by the detailed geometry of the region. We find particularly low [C II]-over-FIR intensity ratios toward large columns of (warm and cold) dust, which suggest the interpretation of the “[C II] deficit” in terms of a “FIR excess”. Conclusions. In terms of the [C II] deficit, we find clear evidence in our data for the importance of [O I] 63 μm emission in the photodissociation regions (PDRs) associated with the Huygens region. A smaller contribution is made by a decreased heating efficiency in regions of high UV irradiation. FIR emission from deeply embedded protostars leads to palpably deficient [C II]/FIR intensity ratios. The [C II] directly associated with the M 42, M 43, and NGC 1977 regions underestimates the star formation rate derived from extragalactic scaling relations. We ascribe this to the importance of [C II] emission from low surface brightness PDR surfaces of molecular clouds which are not included in our survey. Future studies of more active regions of massive star formation will be instrumental in validating the general applicability of these conclusions.

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High-resolution imaging with the International LOFAR Telescope: Observations of the gravitational lenses MG 0751+2716 and CLASS B1600+434

Badole

Venkattu

Jackson

et al. 2022

A&A

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We present Low-Frequency Array (LOFAR) telescope observations of the radio-loud gravitational lens systems MG 0751+2716 and CLASS B1600+434. These observations produce images at 300 milliarcseconds (mas) resolution at 150 MHz. In the case of MG 0751+2716, lens modelling is used to derive a size estimate of around 2 kpc for the low-frequency source, which is consistent with a previous 27.4 GHz study in the radio continuum with Karl G. Jansky Very Large Array (VLA). This consistency implies that the low-frequency radio source is cospatial with the core-jet structure that forms the radio structure at higher frequencies, and no significant lobe emission or further components associated with star formation are detected within the magnified region of the lens. CLASS B1600+434 is a two-image lens where one of the images passes through the edge-on spiral lensing galaxy, and the low radio frequency allows us to derive limits on propagation effects, namely scattering, in the lensing galaxy. The observed flux density ratio of the two lensed images is 1.19±0.04 at an observed frequency of 150 MHz. The widths of the two images give an upper limit of 0.035 kpc m −20/3 on the integrated scattering column through the galaxy at a distance approximately 1 kpc above its plane, under the assumption that image A is not affected by scattering. This is relatively small compared to limits derived through very long baseline interferometry (VLBI) studies of differential scattering in lens systems. These observations demonstrate that LOFAR is an excellent instrument for studying gravitational lenses. We also report on the inability to calibrate three further lens observations: two from early observations that have less well determined station calibration, and a third observation impacted by phase transfer problems.

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Full of Orions: a 200-pc mapping of the interstellar medium in the redshift-3 lensed dusty star-forming galaxy SDP.81

Cited by 37 publications

References 110 publications

High-redshift star formation in the Atacama large millimetre/submillimetre array era

High-redshift star formation in the Atacama large millimetre/submillimetre array era

[C II] 158 μm line emission from Orion A I. A template for extragalactic studies?

High-resolution imaging with the International LOFAR Telescope: Observations of the gravitational lenses MG 0751+2716 and CLASS B1600+434

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Full of Orions: a 200-pc mapping of the interstellar medium in the redshift-3 lensed dusty star-forming galaxy SDP.81

Cited by 37 publications

References 110 publications

High-redshift star formation in the Atacama large millimetre/submillimetre array era

High-redshift star formation in the Atacama large millimetre/submillimetre array era

[C II] 158 μm line emission from Orion A I. A template for extragalactic studies?

High-resolution imaging with the International LOFAR Telescope: Observations of the gravitational lenses MG 0751+2716 and CLASS B1600+434

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[C II] 158 μm line emission from Orion A I. A template for extragalactic studies?