REVIEW 7 cited by
The ALMA-CRISTAL survey: Extended [CII] emission in an interacting galaxy system at z ~ 5.5
Not yet reviewed by Pith; the record is open.
This paper has not been read by Pith yet. Machine review is queued; the pith claim, tier, and objections will appear here once it completes.
SPECIMEN: schema-true, not a live event
T0 review · schema-true
One-sentence machine reading of the paper's core claim.
pith:XXXXXXXX · record.json · timestamp
Signed reviews
read the original abstract
The ALMA [CII] Resolved Ism in STar-forming gALaxies (CRISTAL) survey is a Cycle 8 ALMA Large Programme that studies the cold gas component of high-redshift galaxies. Its sub-arcsecond resolution observations are key to disentangling physical mechanisms that shape galaxies during cosmic dawn. In this paper, we explore the morphology and kinematics of the cold gas, star-forming, and stellar components in the star-forming main-sequence galaxy CRISTAL-05/HZ3, at z = 5.54. Our analysis includes 0.3" spatial resolution (~2 kpc) ALMA observations of the [CII] line. While CRISTAL-05 was previously classified as a single source, our observations reveal that the system is a close interacting pair surrounded by an extended component of carbon-enriched gas. This is imprinted in the disturbed elongated [CII] morphology and the separation of the two components in the position-velocity diagram (~100 km/s). The central region is composed of two components, named C05-NW and C05-SE, with the former being the dominant one. A significant fraction of the [CII] arises beyond the close pair up to 10 kpc, while the regions forming new massive stars and the stellar component seem compact (r_[CII] ~ 4 r_UV), as traced by rest-frame UV and optical imaging obtained with the Hubble Space Telescope and the James Webb Space Telescope. Our kinematic model, using the DYSMALpy software, yields a minor contribution of dark matter of C05-NW within a radius of ~2x Reff. Finally, we explore the resolved [CII]/FIR ratios as a proxy for shock-heating produced by this merger. We argue that the extended [CII] emission is mainly caused by the merger, which could not be discerned with lower-resolution observations. Our work emphasizes the need for high-resolution observations to fully characterize the dynamic stages of infant galaxies and the physical mechanisms that drive the metal enrichment of the circumgalactic medium.
Forward citations
Cited by 7 Pith papers
-
BlackTHUNDER Reveals a Massive Filament around a Compact AGN at $z\simeq5.23$
GN-77652, a compact broad-line AGN at z=5.229, lies beside a 12 kpc multi-source filament at the same redshift whose coalescence will erase the compact AGN appearance within ~150–440 Myr.
-
Fine-structure Line Atlas for Multi-wavelength Extragalactic Study (FLAMES) III: [C II] as Tracer, Crisis of SFR, [O III]/[C II] at High-z, New Answers and New Questions
A universal gas-line deficit relative to infrared luminosity, seen in [C II], [O I], [N II], and extinction-corrected H-alpha, breaks standard SFR calibrations in the brightest dusty galaxies and implies a metallicity...
-
The ALMA-CRISTAL survey: Gas, dust, and stars in star-forming galaxies when the Universe was ~1 Gyr old I. Survey overview and case studies
A spatially resolved ALMA survey of 39 main-sequence galaxies at z~4-6 finds diverse morphologies, an Arp 220-like [CII] deficit, and elevated [CII]/FIR ratios in a previously unexplored surface brightness range.
-
The ALMA-CRISTAL survey: weak evidence for star-formation driven outflows in $z\sim5$ main-sequence galaxies
Stacked ALMA [CII] spectra of 15 z~5 main-sequence galaxies show weak, method-dependent evidence for broad outflow wings, largely attributable to a single known outflow galaxy.
-
The [C II] line emission as an interstellar medium probe in the MARIGOLD galaxies
In simulated high-redshift galaxies, [C II] luminosity traces gas-phase metal mass most tightly, and a calibration that includes recent star formation improves molecular gas estimates by a factor of 2.3.
-
The ALMA-CRISTAL Survey: Complex kinematics of the galaxies at the end of the Reionization Era
HZ10, previously thought to be one massive galaxy at z=5.65, is resolved into at least three interacting components whose [CII] kinematics are consistent with several merger scenarios.
-
Low-redshift analogues of cosmic noon galaxies as laboratories for clumpy star formation
Clumps in low-redshift analogues of high-redshift galaxies are a few hundred parsecs across, and simulated cosmic-noon observations show that clustering and limited resolution inflate their apparent sizes.
Discussion (0). Continue with ORCID to comment.