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VERSION:2.0
CALSCALE:GREGORIAN
PRODID:UW-Madison-Physics-Events
BEGIN:VEVENT
SEQUENCE:1
UID:UW-Physics-Event-9618
DTSTART:20260506T190000Z
DTEND:20260506T210000Z
DTSTAMP:20260413T083718Z
LAST-MODIFIED:20260305T204706Z
LOCATION:Chamberlin 5280
SUMMARY:Identifying and Characterizing Dusty Star-forming Galaxies wit
 h ALMA and JWST\, Thesis Defense\, Stephen McKay
DESCRIPTION:Understanding the formation and evolution of dusty star-fo
 rming galaxies (DSFGs) has been challenging due to the difficulty of r
 eliably identifying them and determining their redshifts and physical 
 properties. In my thesis\, I present several studies using Atacama Lar
 ge Millimeter/submillimeter Array (ALMA) and James Webb Space Telescop
 e (JWST) observations to characterize the DSFG population. First\, I u
 se multiwavelength ALMA continuum observations of 870 μm-selected DSF
 Gs to model their dust spectral energy distributions to high precision
 \, showing that the dust properties of sources at cosmic noon are gene
 rally consistent with those seen in local galaxies and predicted by mo
 dels. Second\, I use a JWST/NIRCam selection to determine accurate pos
 itions for single-dish submillimeter (SCUBA-2) sources and to identify
  faint (S850μm < 2 mJy) DSFGs\, enabling me to probe a lower star-for
 mation rate (SFR) regime (SFR ~ 50-150 Msun/yr)\, below the typical li
 mits of single-dish submillimeter surveys. I measure the physical prop
 erties and morphologies of these DSFGs\, finding that the stellar mass
 es and morphologies of the bright (S850μm > 2 mJy) sources are remark
 ably similar to those of the faint sources. I also observe a low fract
 ion of major mergers in constrast with previous studies based on rest-
 frame optical wavelengths\, suggesting that these studies may have bee
 n impacted by severe dust attenuation. Finally\, I use ALMA linescans 
 along with ancillary JWST and ground-based redshifts to achieve a near
 ly complete spectroscopic redshift distribution for a sample of DSFGs 
 with S850μm > 2.5 mJy for the first time. I use these spectroscopic r
 edshifts to test the effectiveness of various photometric redshift est
 imation methods and to constrain the shape of the DSFG redshift distri
 bution.
URL:https://www.physics.wisc.edu/events/?id=9618
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