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BEGIN:VEVENT
DTSTART;TZID=Atlantic/Canary:20220510T123000
DTEND;TZID=Atlantic/Canary:20220510T133000
UID:iactalks-1581
X-WR-CALNAME: IAC Talks: Open Astronomy Seminars
X-ORIGINAL-URL: /iactalks/Talks/view/1581
CREATED:2022-05-10T12:30:00+01:00
X-WR-CALDESC: IAC Talks upcomming talks
SUMMARY:Dust polarization spectral dependence as major constraint for primo
 rdial CMB B-modes detection
DESCRIPTION:Dust polarization spectral dependence as major constraint for p
 rimordial CMB B-modes detection\nDr. Alessia Ritacco\n\nThe search for the
  primordial B-modes polarization in the cosmic microwave background (CMB) 
 radiation,carrying the signature of the primordial gravitational waves fro
 m the inflation epoch, motivated a significanttechnological progress enabl
 ing the next generation of CMB instruments (e.g. CMB-S4, LiteBIRD)to reach
  an unprecedented sensitivity. However, such a challenging detection deman
 ds a very high controlof the instrumental systematics and CMB foreground e
 missions.Among those, the galactic dust polarized emission spectral depend
 ence, not yet fullycharacterized, could leave a high level of uncertainty 
 in the cosmological polarization dataproducing an ambiguous detection of t
 he CMB B-modes.Characterizing the dust spectral energy distribution (SED) 
 spatial variations became one ofthe most critical issues in the quest for 
 primordial B-modes.In the work that I will present we have used the releas
 e of the Planck satellite HFI dataobtained with the software Sroll2 (Delou
 is+2019, A&A 629, A38), in order to characterizeand compare the SEDs f
 or polarization and total intensity.The mean SEDs for dust polarization an
 d total intensity from 353 to 100 GHz are confirmedto be remarkably close.
  However, the data show evidence for spatial variations of thepolarization
  SED. These variations are correlated with variations of dust temperaturem
 easured on total intensity data but the correlation is tight only in the G
 alactic plane.At higher latitudes, by considering 90% of useful sky fracti
 on and less, the amplitude of the dustemission residuals in polarization s
 uggests that an additional contribution, coming fromvariations of the pola
 rization angle, becomes dominant. Current models, which extrapolatethe SED
  spatial variations from total intensity to polarization, would be therefo
 re grosslysimplifying and underestimating the foreground signal to CMB pol
 arization.\n
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