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

Algera, H. S. B.; Inami, Hanae; Sommovigo, Laura; Fudamoto, Yoshinobu; Schneider, Raffaella; Graziani, Luca; Dayal, Pratika; Aravena, M.; Cunha, Elisabete da; Ferrara, Andrea; Hygate, Alexander P. S.; Leeuwen, Ivana van; Palla, Marco; Pallottini, Andrea; Smit, Renske; Stefanon, Mauro; Topping, Michael W.; Werf, P. van der

doi:10.48550/arxiv.2301.09659

Cited by 8 publications

(7 citation statements)

References 117 publications

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“…high U ion ), high sSFR (i.e., undergoing a bursty event or a young stellar age), high FIR [O iii]/[O i] (i.e., large volume fraction of ionized gas to neutral gas), and low metallicity. The result that high [O iii]/[C ii] shows high ionization parameters and burstiness is consistent with Harikane et al (2020), Sugahara et al (2022), andAlgera et al (2023), respectively. We do not observe a strong correlation between [O iii]/[C ii] and T d (but see Walter et al 2018;Algera et al 2023).…”

Section: Characteristics Of High [O Iii]-to-[c Ii] Galaxiessupporting

confidence: 73%

“…The result that high [O iii]/[C ii] shows high ionization parameters and burstiness is consistent with Harikane et al (2020), Sugahara et al (2022), andAlgera et al (2023), respectively. We do not observe a strong correlation between [O iii]/[C ii] and T d (but see Walter et al 2018;Algera et al 2023). The strongest correlations are found in O 32 (i.e., U ion ) and high FIR [O iii]/[O i] (i.e., the ionized-to-neutral gas volume filling factor), which are in qualitative agreements with the claims of Harikane et al (2020) and Katz et al (2022).…”

Section: Characteristics Of High [O Iii]-to-[c Ii] Galaxiessupporting

confidence: 73%

“…1). At high-z, Carniani et al (2017) have reported that [C ii] is blue-shifted with respect to [O iii] by ∼ 500 km s −1 in the BDF-3299 galaxy at z = 7.2 (see also, e.g., Algera et al 2023 for other high-z examples). The authors have ascribed the velocity offset to a different kinematics of [C ii]-and [O iii]-emitting gas, i.e., predominantly-neutral and the ionized gas phase, respectively.…”

Section: Comparisons Of Line Luminosities To the Literature Samplesmentioning

confidence: 98%

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Detections of [C II] 158 $μ$m and [O III] 88 $μ$m in a Local Lyman Continuum Emitter, Mrk 54, and its Implications to High-redshift ALMA Studies

Ura¹,

Hashimoto²,

Inoue³

et al. 2023

Preprint

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We present integral field, far-infrared (FIR) spectroscopy of Mrk 54, a local Lyman Continuum Emitter (LCE), obtained with FIFI-LS on the Stratospheric Observatory for Infrared Astronomy. This is only the second time, after Haro 11, that [C ii] 158 µm and [O iii] 88 µm spectroscopy of the known LCEs have been obtained. We find that Mrk 54 has a strong [C ii] emission that accounts for ∼ 1% of the total FIR luminosity, whereas it has only moderate [O iii] emission, resulting in the low [O iii]/[C ii] luminosity ratio of 0.22 ± 0.06. In order to investigate whether [O iii]/[C ii] is a useful tracer of f esc (LyC escape fraction), we examine the correlations of [O iii]/[C ii] and (i) the optical line ratio of O 32 ≡ [O iii] 5007 Å/[O ii] 3727 Å, (ii) specific star formation rate, (iii) [O iii] 88 µm/[O i] 63 µm ratio, (iv) gas phase metallicity, and (v) dust temperature based on a combined sample of Mrk 54 and the literature data from the Herschel Dwarf Galaxy Survey and the LITTLE THINGS Survey. We find that galaxies with high [O iii]/[C ii] luminosity ratios could be the result of high ionization (traced by O 32 ), bursty star formation, high ionized-to-neutral gas volume filling factors (traced by [O iii] 88 µm/[O i] 63 µm), and low gas-phase metallicities, which is in agreement with theoretical predictions. We present an empirical relation between the [O iii]/[C ii] ratio and f esc based on the combination of the [O iii]/[C ii] and O 32 correlation, and the known

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Section: Characteristics Of High [O Iii]-to-[c Ii] Galaxiessupporting

confidence: 73%

Section: Characteristics Of High [O Iii]-to-[c Ii] Galaxiessupporting

confidence: 73%

Section: Comparisons Of Line Luminosities To the Literature Samplesmentioning

confidence: 98%

See 1 more Smart Citation

Detections of [C II] 158 $μ$m and [O III] 88 $μ$m in a Local Lyman Continuum Emitter, Mrk 54, and its Implications to High-redshift ALMA Studies

Ura¹,

Hashimoto²,

Inoue³

et al. 2023

Preprint

View full text Add to dashboard Cite

show abstract

Section: Characteristics Of Highsupporting

confidence: 54%

“…shows high ionization parameters and burstiness is consistent with Harikane et al (2020), Sugahara et al (2022), andAlgera et al (2023), respectively. We do not observe a strong correlation between [O III]/[C II] and T d (but see Walter et al 2018;Algera et al 2023). The strongest correlations are found in O 32 (i.e., U ion ) and high FIR [O III]/[O I] (i.e., the ionized-to-neutral gas volume filling factor), which are in qualitative agreement with the claims of Harikane et al (2020) and Katz et al (2022).…”

Section: Characteristics Of Highsupporting

confidence: 54%

Detections of [C ii] 158 μm and [O iii] 88 μm in a Local Lyman Continuum Emitter, Mrk 54, and Its Implications to High-redshift ALMA Studies*

Ura

Hashimoto

Inoue

et al. 2023

ApJ

View full text Add to dashboard Cite

We present integral field, far-infrared (FIR) spectroscopy of Mrk 54, a local Lyman continuum emitter, obtained with FIFI-LS on the Stratospheric Observatory for Infrared Astronomy. This is only the second time, after Haro 11, that [C ii] 158 μm and [O iii] 88 μm spectroscopy of the known LCEs have been obtained. We find that Mrk 54 has a strong [C ii] emission that accounts for ∼1% of the total FIR luminosity, whereas it has only moderate [O iii] emission, resulting in the low [O iii]/[C ii] luminosity ratio of 0.22 ± 0.06. In order to investigate whether [O iii]/[C ii] is a useful tracer of f esc (LyC escape fraction), we examine the correlations of [O iii]/[C ii] and (i) the optical line ratio of O32 ≡ [O iii] 5007 Å/[O ii] 3727 Å, (ii) specific star formation rate, (iii) [O iii] 88 μm/[O i] 63 μm ratio, (iv) gas-phase metallicity, and (v) dust temperature based on a combined sample of Mrk 54 and the literature data from the Herschel Dwarf Galaxy Survey and the LITTLE THINGS Survey. We find that galaxies with high [O iii]/[C ii] luminosity ratios could be the result of high ionization (traced by O32), bursty star formation, high ionized-to-neutral gas volume filling factors (traced by [O iii] 88 μm/[O i] 63 μm), and low gas-phase metallicities, which is in agreement with theoretical predictions. We present an empirical relation between the [O iii]/[C ii] ratio and f esc based on the combination of the [O iii]/[C ii] and O32 correlation, and the known relation between O32 and f esc. The relation implies that high-redshift galaxies with high [O iii]/[C ii] ratios revealed by the Atacama Large Millimeter/submillimeter Array may have f esc ≳ 0.1, significantly contributing to the cosmic reionization.

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The ALMA REBELS Survey: discovery of a massive, highly star-forming, and morphologically complex ULIRG at z = 7.31

Hygate

Hodge

Cunha

et al. 2023

Monthly Notices of the Royal Astronomical Society

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We present Atacama Large Millimeter/Submillimeter Array (ALMA) [C ii] and ∼158 $\rm \mu m$ continuum observations of REBELS-25, a massive, morphologically complex ultra-luminous infrared galaxy (ULIRG; LIR = $1.5^{+0.8}_{-0.5} \times 10^{12}$ L⊙) at z = 7.31, spectroscopically confirmed by the Reionization Era Bright Emission Line Survey (REBELS) ALMA Large Programme. REBELS-25 has a significant stellar mass of $M_{*} = \mbox{$ 8^{+4}_{-2} \times 10^{9} $}{} ~\mbox{M$_\odot $}{}$. From dust-continuum and ultraviolet observations, we determine a total obscured + unobscured star formation rate of SFR $= \mbox{$199^{+101}_{-63}$}{} ~ \mbox{M$_\odot $}~ {-1}$. This is about four times the SFR estimated from an extrapolated main-sequence. We also infer a [C ii]-based molecular gas mass of $M_{{\rm H}_{2}} = \mbox{$5.1^{+5.1}_{-2.6} \times 10^{10}$}{} ~\mbox{M$_\odot $}{}$, implying a molecular gas depletion time of $t_{\rm depl, {\rm H}_{2}} = \mbox{$0.3^{+0.3}_{-0.2} $}{}$ Gyr. We observe a [C ii] velocity gradient consistent with disc rotation, but given the current resolution we cannot rule out a more complex velocity structure such as a merger. The spectrum exhibits excess [C ii] emission at large positive velocities (∼500 km s−1), which we interpret as either a merging companion or an outflow. In the outflow scenario, we derive a lower limit of the mass outflow rate of 200 M⊙ − 1, which is consistent with expectations for a star formation-driven outflow. Given its large stellar mass, SFR and molecular gas reservoir ∼700 Myr after the Big Bang, we explore the future evolution of REBELS-25. Considering a simple, conservative model assuming an exponentially declining star formation history, constant star formation efficiency, and no additional gas inflow, we find that REBELS-25 has the potential to evolve into a galaxy consistent with the properties of high-mass quiescent galaxies recently observed at z ∼ 4.

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

Cited by 8 publications

References 117 publications

Detections of [C II] 158 $μ$m and [O III] 88 $μ$m in a Local Lyman Continuum Emitter, Mrk 54, and its Implications to High-redshift ALMA Studies

Detections of [C II] 158 $μ$m and [O III] 88 $μ$m in a Local Lyman Continuum Emitter, Mrk 54, and its Implications to High-redshift ALMA Studies

Detections of [C ii] 158 μm and [O iii] 88 μm in a Local Lyman Continuum Emitter, Mrk 54, and Its Implications to High-redshift ALMA Studies*

The ALMA REBELS Survey: discovery of a massive, highly star-forming, and morphologically complex ULIRG at z = 7.31

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