Internal Structure of Molecular Gas in a Main-sequence Galaxy With a UV Clump at z = 1.45

Ushio, Kaito; Ohta, Kouji; Maeda, Fumiya; Hatsukade, Bunyo; Yabe, Kiyoto

doi:10.3847/1538-4357/abdd1f

Cited by 4 publications

(15 citation statements)

References 61 publications

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“…The Cosmic Snake and A521 both appear to be different from other high-redshift galaxies that we can use for a more direct comparison with contemporary galaxies: the scale lengths reported for the MS galaxy at z = 1.45 by Ushio et al (2021) and for the stacks of galaxies at z > 0.1 (Jafariyazani et al 2019;Calistro Rivera et al 2018) are shorter than in A521 and longer than in the Cosmic Snake for all three physical quantities. Altogether, this suggests that l mol , l SFR , and l of high-redshift (z = 0.1 − 3) galaxies cover a similarly wide range of values as in local galaxies.…”

Section: Comparison Of Radial Profiles With Local Galaxies and Other ...mentioning

confidence: 74%

“…The derived HLR of the Cosmic Snake and A521 are typical of galaxies at z ∼ 1 with comparable M (see e.g. van der Wel et al 2014). We then used the radial profile of ΣM to compute µ HLR , and we find (5.2 ± 0.5) × 10 8 M kpc −2 for the Cosmic Snake and (4.9 ± 0.2) × 10 8 M kpc −2 for A521.…”

Section: Morphological Parameters Of the Cosmic Snake And A521mentioning

confidence: 90%

“…We considered 52 local galaxies, including 15 galaxies from Regan et al (2001), 14 from Tamburro et al (2008), and 23 from Leroy et al (2008). We also compared them with high-redshift galaxies with published radial profiles: a massive (1.2 +0.3 −0.2 × 10 11 M ) MS galaxy at z = 1.45 from Ushio et al (2021), a stack of 32 galaxies at z = 0.1 − 0.42 from Jafariyazani et al ( 2019), and a stack of 4 sub-millimetre galaxies at z ∼ 2−3 from Calistro Rivera et al (2018). To trace the molec-ular gas, Regan et al (2001) used the CO(1-0) emission line, whereas Leroy et al (2008) used the CO(2-1) emission in all but two galaxies (NGC 3627 and NGC 5194), where they used the CO(1-0) emission.…”

Section: Comparison Of Radial Profiles With Local Galaxies and Other ...mentioning

confidence: 99%

“…To trace the molec-ular gas, Regan et al (2001) used the CO(1-0) emission line, whereas Leroy et al (2008) used the CO(2-1) emission in all but two galaxies (NGC 3627 and NGC 5194), where they used the CO(1-0) emission. Ushio et al (2021) used the CO(2-1) emission line, and Calistro Rivera et al (2018) used the CO(3-2) emission line.…”

Section: Comparison Of Radial Profiles With Local Galaxies and Other ...mentioning

confidence: 99%

“…For both galaxies, we combine observations obtained with HST and ALMA and observations of the Cosmic Snake obtained with SINFONI and the Herschel space observatory in order to measure the radial profiles of their surface densities of SFR (ΣSFR), M (ΣM ), M mol (ΣM mol ), and M dust (ΣM dust ), and the corresponding scale lengths (assuming an exponential profile). We compare these radial profiles with those of 52 nearby galaxies from studies by Regan et al (2001), Leroy et al (2008), andTamburro et al (2008), as well as one individual galaxy at z = 1.45 from Ushio et al (2021), and two stacks obtained for the high-redshift galaxies analysed in Calistro Rivera et al ( 2018) (z ∼ 2 − 3) and in Jafariyazani et al (2019)…”

Section: Introductionmentioning

confidence: 99%

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Radial profiles of lensed $z \sim 1$ galaxies on sub-kiloparsec scales

Nagy,

Dessauges-Zavadsky,

Richard

et al. 2021

Preprint

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We study the spatially resolved physical properties of the Cosmic Snake arc in MACS J1206.2-0847 and the arc in Abell 0521 (A521). These are two strongly lensed galaxies at redshifts z = 1.036 and z = 1.044. We used observations of the Hubble Space Telescope (HST) and the Atacama Large Millimeter/submillimeter Array (ALMA). The former gives access to the star formation rate (SFR) and stellar mass (M ), and the latter to the H 2 molecular gas mass (M mol ). HST and ALMA observations have similar angular resolutions of 0.15 − 0.2 , which with the help of strong gravitational lensing enable us to reach spatial resolutions down to ∼ 30 pc and ∼ 100 pc in these two galaxies, respectively. These resolutions are close to the resolution of observations of nearby galaxies. We study the radial profiles of SFR, M , and M mol surface densities of these high-redshift galaxies and compare the corresponding exponential scale lengths with those of local galaxies. We find that the scale lengths in the Cosmic Snake are about 0.5 kpc − 1.5 kpc, and they are 3 to 10 times larger in A521. This is a significant difference knowing that the two galaxies have comparable integrated properties. These high-redshift scale lengths are nevertheless comparable to those of local galaxies, which cover a wide distribution. The particularity of our high-redshift radial profiles is the normalisation of the M mol surface density profiles (ΣM mol ), which are offset by up to a factor of 20 with respect to the profiles of z = 0 counterparts. The SFR surface density profiles are also offset by the same factor as ΣM mol , as expected from the Kennicutt-Schmidt law.

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Section: Comparison Of Radial Profiles With Local Galaxies and Other ...mentioning

confidence: 74%

Section: Morphological Parameters Of the Cosmic Snake And A521mentioning

confidence: 90%

Section: Comparison Of Radial Profiles With Local Galaxies and Other ...mentioning

confidence: 99%

Section: Comparison Of Radial Profiles With Local Galaxies and Other ...mentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Radial profiles of lensed $z \sim 1$ galaxies on sub-kiloparsec scales

Nagy,

Dessauges-Zavadsky,

Richard

et al. 2021

Preprint

View full text Add to dashboard Cite

show abstract

Radial profiles of lensed z ∼ 1 galaxies on sub-kiloparsec scales

Nagy

Dessauges‐Zavadsky

Richard

et al. 2021

A&A

View full text Add to dashboard Cite

We study the spatially resolved physical properties of the Cosmic Snake arc in MACS J1206.2–0847 and the arc in Abell 0521 (A521). These are two strongly lensed galaxies at redshifts z = 1.036 and z = 1.044. We used observations of the Hubble Space Telescope (HST) and the Atacama Large Millimeter/submillimeter Array (ALMA). The former gives access to the star formation rate (SFR) and stellar mass (M⋆), and the latter to the H2 molecular gas mass (Mmol). HST and ALMA observations have similar angular resolutions of 0.15″ − 0.2″, which with the help of strong gravitational lensing enable us to reach spatial resolutions down to ∼30 pc and ∼100 pc in these two galaxies, respectively. These resolutions are close to the resolution of observations of nearby galaxies. We study the radial profiles of SFR, M⋆, and Mmol surface densities of these high-redshift galaxies and compare the corresponding exponential scale lengths with those of local galaxies. We find that the scale lengths in the Cosmic Snake are about 0.5 kpc − 1.5 kpc, and they are 3–10 times larger in A521. This is a significant difference knowing that the two galaxies have comparable integrated properties. These high-redshift scale lengths are nevertheless comparable to those of local galaxies, which cover a wide distribution. The particularity of our high-redshift radial profiles is the normalisation of the Mmol surface density profiles (ΣMmol), which are offset by up to a factor of 20 with respect to the profiles of z = 0 counterparts. The SFR surface density profiles are also offset by the same factor as ΣMmol, as expected from the Kennicutt-Schmidt law.

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Unveiling [C II] clumps in a lensed star-forming galaxy at z ∼ 3.4

Zanella,

Iani,

Dessauges-Zavadsky

et al. 2024

A&A

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Observations at UV and optical wavelengths have revealed that galaxies at $z 1 - 4$ host star-forming regions, dubbed ``clumps,'' which are believed to form due to the fragmentation of gravitationally unstable, gas-rich disks. However, the detection of the parent molecular clouds that give birth to such clumps is still possible only in a minority of galaxies, mostly at $z We investigated the and dust morphology of a $z 3.4$ lensed galaxy hosting four clumps detected in the UV continuum. We aimed to observe the emission of individual clumps that, unlike the UV, is not affected by dust extinction, to probe their nature and cold gas content. We conducted ALMA observations probing scales down to $ 300$ pc and detected three clumps. One (dubbed ``NE'') coincides with the brightest UV clump, while the other two (``SW'' and ``C'') are not detected in the UV continuum. We do not detect the dust continuum. We converted the luminosity of individual clumps into molecular gas mass and found $ M_ mol 10^8\, M_ odot $. By complementing it with the star formation rate (SFR) estimate from the UV continuum, we estimated the gas depletion time ($t_ dep $) of clumps and investigated their location in the Schmidt-Kennicutt plane. While the NE clump has a very short $t_ dep Gyr $, which is comparable with high-redshift starbursts, the SW and C clumps instead have longer $t_ dep Gyr $ and are likely probing the initial phases of star formation. The lack of dust continuum detection is consistent with the blue UV continuum slope estimated for this galaxy ($ -2.5$) and it indicates that dust inhomogeneities do not significantly affect the detection of UV clumps in this target. We pushed the observation of the cold gas content of individual clumps up to $z 3.4$ and showed that the line emission is a promising tracer of molecular clouds at high redshift, allowing the detection of clumps with a large range of depletion times.

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Internal Structure of Molecular Gas in a Main-sequence Galaxy With a UV Clump at z = 1.45

Cited by 4 publications

References 61 publications

Radial profiles of lensed $z \sim 1$ galaxies on sub-kiloparsec scales

Radial profiles of lensed $z \sim 1$ galaxies on sub-kiloparsec scales

Radial profiles of lensed z ∼ 1 galaxies on sub-kiloparsec scales

Unveiling [C II] clumps in a lensed star-forming galaxy at z ∼ 3.4

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