Arp 220: A Post-starburst Galaxy with Little Current Star Formation outside of Its Nuclear Disks

Chandar, Rupali; Caputo, Miranda; Linden, Sean T.; Mok, Angus; Whitmore, Bradley C.; Calzetti, Daniela; Elmegreen, D. M.; Lee, Janice; Úbeda, Leonardo; White, R. L.; Cook, D.

doi:10.3847/1538-4357/acac96

Cited by 6 publications

(1 citation statement)

References 77 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Morphological analysis based on 1– m PRIMER and CEERS imaging of our galaxies rule out any secondary reddened components for our sources (e.g. 60 , 61 ). A detailed JWST/NIRcam morphological analysis of the S18 sources will be presented by Kawinwanichakij et al (in prep).…”

Section: Resultsmentioning

confidence: 74%

A population of faint, old, and massive quiescent galaxies at $$3<z<4$$ revealed by JWST NIRSpec Spectroscopy

Nanayakkara,

Glazebrook,

Jacobs

et al. 2024

Sci Rep

View full text Add to dashboard Cite

Here we present a sample of 12 massive quiescent galaxy candidates at $$z\sim 3-4$$ z ∼ 3 - 4 observed with the James Webb Space Telescope (JWST) Near Infrared Spectrograph (NIRSpec). These galaxies were pre-selected from the Hubble Space Telescope imaging and 10 of our sources were unable to be spectroscopically confirmed by ground based spectroscopy. By combining spectroscopic data from NIRSpec with multi-wavelength imaging data from the JWST Near Infrared Camera (NIRCam), we analyse their stellar populations and their formation histories. We find that all of our galaxies classify as quiescent based on the reconstruction of their star formation histories but show a variety of quenching timescales and ages. All our galaxies are massive ($$\sim 0.1-1.2\times 10^{11}$$ ∼ 0.1 - 1.2 × 10 11 M$$_\odot$$ ⊙ ), with masses comparable to massive galaxies in the local Universe. We find that the oldest galaxy in our sample formed $$\sim 1.0\times 10^{11}$$ ∼ 1.0 × 10 11 M$$_\odot$$ ⊙ of mass within the first few hundred million years of the Universe and has been quenched for more than a billion years by the time of observation at $$z\sim 3.2$$ z ∼ 3.2 ($$\sim 2$$ ∼ 2 billion years after the Big Bang). Our results point to very early formation of massive galaxies requiring a high conversion rate of baryons to stars in the early Universe.

show abstract

Section: Resultsmentioning

confidence: 74%

A population of faint, old, and massive quiescent galaxies at $$3<z<4$$ revealed by JWST NIRSpec Spectroscopy

Nanayakkara,

Glazebrook,

Jacobs

et al. 2024

Sci Rep

View full text Add to dashboard Cite

show abstract

JWST/CEERS sheds light on dusty star-forming galaxies: Forming bulges, lopsidedness, and outside-in quenching at cosmic noon

Le Bail,

Daddi,

Elbaz

et al. 2024

A&A

View full text Add to dashboard Cite

We investigate the morphology and resolved physical properties of a sample of 22 IR-selected dusty star-forming galaxies at cosmic noon using the James Webb Space Telescope NIRCam images obtained in the EGS field for the CEERS survey. The exceptional resolution of the NIRCam images allowed us to spatially resolve these galaxies up to $4.4 and identify their bulge or core even when very extinguished by dust. The goal of this study is to obtain a better understanding of the formation and evolution of FIR-bright galaxies by spatially resolving their properties using JWST in order to look through the dust and bridge the gap between the compact FIR sources and the larger optical star-forming galaxies. Based on red-green-blue images from the F115W, F200W, and F444W filters, we divided each galaxy into several uniformly colored regions, fit their respective SEDs, and measured physical properties. After classifying each region as star forming or quiescent, we assigned galaxies to three classes depending on whether active star formation is located in the core, in the disk, or in both. (i) We find that the galaxies at a higher redshift tend to have a fragmented disk with a low core mass fraction. They are at an early stage of bulge formation. When moving toward a lower redshift, the core mass fraction increases, and the bulge growth is associated with a stabilization of the disk, which translates into less patches and clumps. The NIRCam data clearly point toward bulge formation in preexisting disks (ii) Lopsidedness is a very common feature of DSFGs. It has been wrongly overlooked for a long time and could have a major impact on the evolution of DSFGs. (iii) Twenty-three percent of the galaxies have a star-forming core embedded in a quiescent disk. They seem to be undergoing outside-in quenching, often facilitated by their strong lopsidedness inducing instabilities. (iv) We show that half of our galaxies with star formation concentrated in their core are good sub-millimeter galaxy near-IR counterpart candidates, demonstrating that compact SMGs are usually surrounded by a larger, less obscured disk. (v) Finally, we found surprising evidence for clump-like substructures being quiescent or residing in quiescent regions. This work demonstrates the major impact JWST/NIRCam has on understanding the complexity of the evolution of distant massive galaxies regarding bulge formation and quenching mechanisms.

show abstract

No evidence of active galactic nucleus features in the nuclei of Arp 220 from JWST/NIRSpec IFS

Perna,

Arribas,

Lamperti

et al. 2024

A&A

View full text Add to dashboard Cite

Arp 220 is the nearest ultra-luminous infrared galaxy. It shows evidence of 100 pc scale molecular outflows that are likely connected with galaxy-scale outflows traced by ionised and neutral gas. The two highly obscured nuclei of Arp 220 are sites of intense star formation, with extreme (far-infrared based) star formation rate surface densities, $ SFR $. Despite extensive investigations that searched for active galactic nucleus (AGN) activity in the Arp 220 nuclei, direct evidence remains elusive. We present JWST/NIRSpec integral field spectroscopy (IFS) observations covering the $0.9-5.1 wavelength range of the innermost ($5 i.e. $1.8 1.5$ kpc) regions of Arp 220. The primary goal is to investigate the potential presence of AGN signatures in the nuclear regions by analysing the spectra extracted from circular apertures with a radius of 55 pc (0.15 around each of the two nuclei. The analysis aims to identify highly ionised gas emission lines (with ionisation potential $> 54$ eV) and other spectral features indicative of AGN activity. Atomic and molecular gas kinematics were also taken into account to study the outflow signatures at $< 60$ pc scales. We identify $ 70$ atomic and $ 50$ molecular emission lines in the nuclear spectra of Arp 220. We used recombination line ratios to measure optical extinctions in the range A$_V 11-14$ mag. High-ionisation lines are not detected, except for the line at 4.49$ which we interpret as due to shocks rather than to AGN ionisation. We identify broadening and multiple kinematic components in the and H$_2$ lines caused by outflows and shocks, with velocities up to $ Significantly higher velocities (up to $ are detected in the off-nuclear regions, but they do not conclusively represent direct evidence for AGN activity. Broad-line region components are not detected in any permitted emission line within the NIRSpec wavelength range. Even with the unprecedented sensitivity of JWST/NIRSpec IFS, achieving an unambiguous identification or exclusion of the presence of an AGN in the Arp 220 system remains challenging because of its extreme dust obscuration.

show abstract

Arp 220: A Post-starburst Galaxy with Little Current Star Formation outside of Its Nuclear Disks

Cited by 6 publications

References 77 publications

A population of faint, old, and massive quiescent galaxies at $$3<z<4$$ revealed by JWST NIRSpec Spectroscopy

A population of faint, old, and massive quiescent galaxies at $$3<z<4$$ revealed by JWST NIRSpec Spectroscopy

JWST/CEERS sheds light on dusty star-forming galaxies: Forming bulges, lopsidedness, and outside-in quenching at cosmic noon

No evidence of active galactic nucleus features in the nuclei of Arp 220 from JWST/NIRSpec IFS

Contact Info

Product

Resources

About