ALMA Reveals Extended Cool Gas and Hot Ionized Outflows in a Typical Star-forming Galaxy at Z = 7.13

Akins, Hollis B.; Fujimoto, Seiji; Finlator, Kristian; Watson, Derrick G.; Knudsen, K. K.; Richard, Johan; Bakx, Tom J. L. C.; Hashimoto, T.; Inoue, Akio; Matsuo, Hiroshi; Michalowski, Michal; Tamura, Yoichi

doi:10.3847/1538-4357/ac795b

Cited by 27 publications

(21 citation statements)

References 104 publications

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“…The dust temperature drops with increasing radius as seen in the top-left panel. A similar dependence is found in a star-forming galaxy at z = 7.13 (Akins et al 2022). We fit a power law, T dust ∝ r −0.41±0.20 .…”

Section: Dust Diagnosticsupporting

confidence: 79%

The interstellar medium distribution, gas kinematics, and system dynamics of the far-infrared luminous quasar SDSS J2310+1855 atz= 6.0

Shao

Wang

Weiß

et al. 2022

A&A

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We present Atacama Large Millimeter/submillimeter Array (ALMA) sub-kiloparsec-to kiloparsec-scale resolution observations of the [C ii], CO (9-8), and OH + (1 1 -0 1 ) lines along with their dust continuum emission toward the far-infrared (FIR) luminous quasar SDSS J231038.88+185519.7 at z = 6.0031, to study the interstellar medium distribution, the gas kinematics, and the quasar-host system dynamics. We decompose the intensity maps of the [C ii] and CO (9-8) lines and the dust continuum with two-dimensional elliptical Sérsic models. The [C ii] brightness follows a flat distribution with a Sérsic index of 0.59. The CO (9-8) line and the dust continuum can be fit with an unresolved nuclear component and an extended Sérsic component with a Sérsic index of ∼1, which may correspond to the emission from an active galactic nucleus dusty molecular torus and a quasar host galaxy, respectively. The different [C ii] spatial distribution may be due to the effect of the high dust opacity, which increases the FIR background radiation on the [C ii] line, especially in the galaxy center, significantly suppressing the [C ii] emission profile. The dust temperature drops with distance from the center. The effective radius of the dust continuum is smaller than that of the line emission and the dust mass surface density, but is consistent with that of the star formation rate surface density. This may indicate that the dust emission is a less robust tracer of the dust and gas distribution but is a decent tracer of the obscured star formation activity. The OH + (1 1 -0 1 ) line shows a P-Cygni profile with an absorption at ∼-400 km/s, which may indicate an outflow with a neutral gas mass of (6.2 ± 1.2) × 10 8 M along the line of sight. We employed a three-dimensional tilted ring model to fit the [C ii] and CO (9-8) data cubes. The two lines are both rotation dominated and trace identical disk geometries and gas motions. This suggest that the [C ii] and CO (9-8) gas are coplanar and corotating in this quasar host galaxy. The consistent circular velocities measured with [C ii] and CO (9-8) lines indicate that these two lines trace a similar gravitational potential. We decompose the circular rotation curve measured from the kinematic model fit to the [C ii] line into four matter components (black hole, stars, gas, and dark matter). The quasar-starburst system is dominated by baryonic matter inside the central few kiloparsecs. We constrain the black hole mass to be 2.97 +0.51 −0.77 × 10 9 M ; this is the first time that the dynamical mass of a black hole has been measured at z ∼ 6. This mass is consistent with that determined using the scaling relations from quasar emission lines. A massive stellar component (on the order of 10 9 M ) may have already existed when the Universe was only ∼0.93 Gyr old. The relations between the black hole mass and the baryonic mass of this quasar indicate that the central supermassive black hole may have formed before its host galaxy.

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Section: Dust Diagnosticsupporting

confidence: 79%

The interstellar medium distribution, gas kinematics, and system dynamics of the far-infrared luminous quasar SDSS J2310+1855 atz= 6.0

Shao

Wang

Weiß

et al. 2022

A&A

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“…We caution, however, that the spectroscopic blueshift and the ≈2σ spatial offset of [C II] relative to the UV component and [O III] emission (Fujimoto et al 2022b) indicate that the origin of the [C II] emission is not fully co-spatial with the most intense, star-forming region of the galaxy. Such extended, blueshifted [C II] emission has been observed in other high-z galaxies, and may hint at an offsetan abundant gas reservoir, a shock-heated outflowing gas, or minor mergers (e.g., Maiolino et al 2015;Kohandel et al 2019;Arata et al 2020;Akins et al 2022;Katz et al 2022). The latter scenario would typically produce much broader (>1000 km s −1 ) [C II] line profiles (Appleton et al 2013), whereas the observed narrow-line feature is consistent with the low stellar mass of S04590.…”

Section: The Total Dynamical Masssupporting

confidence: 63%

“…We (Smit et al 2018;Fujimoto et al 2019;Matthee et al 2019;Carniani et al 2020;Akins et al 2022;Fudamoto et al 2022), though S04590 presents one of the most notable cases with r e,[CII] ≈ 10 × r e,UV . Assuming the "disk" diameter is D [CII] = 2 × r e,[CII] , we infer D [CII] = 2.2 ± 1.4 kpc.…”

Section: The Total Dynamical Massmentioning

confidence: 99%

The Gas and Stellar Content of a Metal-poor Galaxy at z = 8.496 as Revealed by JWST and ALMA

Heintz

Giménez-Arteaga

Fujimoto

et al. 2023

ApJL

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We present a joint analysis of the galaxy S04590 at z = 8.496 based on NIRSpec, NIRCam, and NIRISS observations obtained as part of the Early Release Observations program of the James Webb Space Telescope (JWST) and the far-infrared [C ii] 158 μm emission line detected by dedicated Atacama Large Millimeter/submillimeter Array (ALMA) observations. We determine the physical properties of S04590 from modeling of the spectral energy distribution (SED) and through the redshifted optical nebular emission lines detected with JWST/NIRSpec. The best-fit SED model reveals a low-mass (M ⋆ = 107.2–108 M ⊙) galaxy with a low oxygen abundance of 12 + log ( O / H ) = 7.16 − 0.12 + 0.10 derived from the strong nebular and auroral emission lines. Assuming that [C ii] effectively traces the interstellar medium, we estimate the total gas mass of the galaxy to be M gas = (8.0 ± 4.0) × 108 M ⊙ based on the luminosity and spatial extent of [C ii]. This yields an exceptionally high gas fraction, f gas = M gas/(M gas + M ⋆) ≳ 90%, though one still consistent with the range expected for low metallicity. We further derive the metal mass of the galaxy based on the gas mass and gas-phase metallicity, which we find to be consistent with the expected metal production from Type II supernovae. Finally, we make the first constraints on the dust-to-gas (DTG) and dust-to-metal (DTM) ratios of galaxies in the epoch of reionization at z ≳ 6, showing overall low mass ratios of logDTG < −3.8 and logDTM < −0.5, though they are consistent with established scaling relations and in particular with those of the local metal-poor galaxy I Zwicky 18. Our analysis highlights the synergy between ALMA and JWST in characterizing the gas, metal, and stellar content of the first generation of galaxies.

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“…While [CII] emission in distant galaxies has been observed to be more spatially extended than the [OIII] emission (e.g., Carniani et al 2020;Akins et al 2022; Section 6.1), we note that our results remain unchanged if we re-extract the [CII] fluxes following the procedure adopted for the [OIII] line described in Section 3. This is as expected, given that the fluxes are extracted in an aperture with a radius of ∼ 10 kpc at 𝑧 = 7, which is much larger than the typical [CII] sizes of galaxies of 𝑟 [CII] ∼ 2 kpc (Fujimoto et al 2020;Fudamoto et al 2022b).…”

Section: [Oiii] Emissionmentioning

confidence: 58%

Cold Dust and Low [OIII]/[CII] Ratios: an Evolved Star-forming Population at Redshift 7

Algera¹,

Inami²,

Sommovigo³

et al. 2023

Preprint

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We present new ALMA Band 8 (rest-frame 90 𝜇m) observations of three massive (𝑀 ★ ≈ 10 10 𝑀 ) galaxies at 𝑧 ≈ 7 previously detected in [CII]158 𝜇m and underlying dust continuum emission in the Reionization Era Bright Emission Line Survey (REBELS). We detect the dust continuum emission of two of our targets in Band 8 (REBELS-25 and REBELS-38), while REBELS-12 remains undetected. Through modified blackbody fitting we determine cold dust temperatures (𝑇 dust ≈ 30 − 35 K) in both of the dual-band detected targets, given a fiducial model of optically thin emission with 𝛽 = 2.0. Their dust temperatures are lower than most 𝑧 ∼ 7 galaxies in the literature, and consequently their dust masses are higher (𝑀 dust ≈ 10 8 𝑀 ). Nevertheless, these large dust masses are still consistent with predictions from models of dust production in the early Universe. In addition, we target and detect [OIII]88 𝜇m emission in both REBELS-12 and REBELS-25, and find 𝐿 [OIII] /𝐿 [CII] ratios of approximately unity, low compared to the 𝐿 [OIII] /𝐿 [CII] 2 − 10 observed in the known 𝑧 6 population thus far. We argue the lower line ratios are due to a comparatively weaker ionizing radiation field resulting from the less starbursty nature of our targets. This low burstiness supports the cold dust temperatures and below average [OIII]𝜆𝜆4959, 5007 + H𝛽 equivalent widths of REBELS-25 and REBELS-38, compared to the known high-redshift population. Overall, this provides evidence for the existence of a massive, dust-rich galaxy population at 𝑧 ≈ 7 which has previously experienced vigorous star formation, but is currently forming stars in a steady, as opposed to bursty, manner.

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ALMA Reveals Extended Cool Gas and Hot Ionized Outflows in a Typical Star-forming Galaxy at Z = 7.13

Cited by 27 publications

References 104 publications

The interstellar medium distribution, gas kinematics, and system dynamics of the far-infrared luminous quasar SDSS J2310+1855 atz= 6.0

The interstellar medium distribution, gas kinematics, and system dynamics of the far-infrared luminous quasar SDSS J2310+1855 atz= 6.0

The Gas and Stellar Content of a Metal-poor Galaxy at z = 8.496 as Revealed by JWST and ALMA

Cold Dust and Low [OIII]/[CII] Ratios: an Evolved Star-forming Population at Redshift 7

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