SDSS-II SN Survey: SNe & Hosts

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SDSS-II SN Survey: SNe & Hosts. and the SDSS-II SN collaboration. Peter Garnavich Notre Dame. KITP/UCSB March 23, 2007. Fermilab F. DeJongh, J. Marriner, D. McGinnis, G. Miknaitis U. Chicago B. Dilday, R. Kessler
SDSS-II SN Survey: SNe & Hostsand the SDSS-II SN collaboration
  • Peter Garnavich
  • Notre Dame
  • KITP/UCSB March 23, 2007Fermilab F. DeJongh, J. Marriner, D. McGinnis, G. MiknaitisU. Chicago B. Dilday, R. KesslerAPO H. Brewington, J. Dembicky, M. Harvanek, J. Krzesinski, B. Ketzeback, D. Long, O. Malanushenko, V. Malanushenko, R. McMillan, K. Pan, G. Saurage, S. Snedden, S. WattersSAAO B. Bassett, K. van der HeydenU. Washington A. Becker, C. HoganU. Munich R. Bender, U. HoppSeoul Natl. U. C. Choi, M. ImWayne State U. D. CinabroOhio State U. D. L. DePoy, J. L. PrietoU. Tokyo M. Doi, K. Konishi, T. Morokuma, N. Takanashi, K. Tokita, N. YasudaU. Notre Dame P. Garnavich, J. Gallagher, B.TuckerNM State U. J. HoltzmanKIPAC/Stanford S. Jha, R. Romani, C. ZhengU. Göttingen W. KollatschnySTScI H. Lampeitl, A. RiessU. Portsmouth R. Nichol, M. SmithRochester IT M. RichmondU. Pennsylvania M. SakoPenn State U. D. SchneiderU. Texas C. WheelerJ. Friemanwith help from: J. Eastman, L. Watson, R. Assef,K. Schlesinger, A. Crotts, M. Stritzinger,J. Sollerman, A. Goobar, G. Leloudas, R. J. Foley, A. V. Filippenko, A. Aragon-Salamanca, M. Bremer, M. Turatto, P. Ruiz-Lapuente,F. Castander, A. Romer, C. Collins, J. Lucey, A. Edge, Y. IharaSDSS-II SN Collaboration Main goals of the SDSS SN survey: =>fill in the SN Ia Hubble diagram at intermediate redshift, 0.1 ≲ z ≲ 0.3=>connect low-z with high-z=>confirm concordance cosmology (or not!)=>create a large, uniform sample of well-studied SNIachallenges=>peak magnitudes m ≃ 20-22=>need to search hundreds of deg2➔ SDSS 2.5m telescope + imager Ia Hubble DiagramRiess et al. “Gold Sample”High-Z + SCPSNLS, ESSENCELow-z:Calan-TololoRiess et al.Jha et al.Hamuy et al. (1996),Riess et al. (1999),Jha et al. (2006), ...searchtemplatediffgriM. Sako, U. PennsylvaniaSN 2006fzSN Ia z = 0.105APO 3.5m DIS spectrumBassett et al. (2007), CBET 627continual web page updatesfollow-up is encouraged!J. Marriner, Fermilab452 supernovaespectroscopic SN Ia (313)probable SN Iacore-collapse SNM. Sako, U. PennsylvaniaA. Becker, U. Washingtonfor the first time we have a continuous expansion history measured from SN to z > 1SDSS SN Hubble diagramfrom fall 2005 data(129 SN Ia in all, 74 “clean”)>300 total for 2005+06H. Lampeitl, STScIESSENCE 2007SDSS Finds Unusual Events:SN 2005gj is an example. SN Ia (?) in a dense circumstellar environment.Brighter than 2002ic and smooth decline (SDSS+CSP have a great light curve!)Interaction from the start so mistaken for a IIn at first.Prieto et al.SN 2006gj Looks Like a Type IaVery good spectral fit to 91T + continuum. See Si II and S II characteristic of Ia. More out there: SN 7017Clone of 06gj at z=0.27Parent et al.SDSS-IIMLCS2k2 light-curve fitsJha, Riess, & Kirshner (2007, ApJ, in press)SN 2005ij z = 0.124SN 2005ji z = 0.214SN 2005fs z = 0.344SDSS Supernova/Host Characteristics:2005: >100 well-observed supernovae, uniform discovery & analysisSDSS is “Democratic” - find SN in all types of galaxies
  • Decline Rate (luminosity)
  • Extinction Distribution
  • Host Galaxy Luminosity (number of stars)
  • Host Galaxy Color (Star Formation Rate)
  • Hubble Residuals
  • Galactocentric Distance Extinction Host SFR
  • Relative SN Rate by Host SFR
  • B. Dilday, U. ChicagoLuminosity vs Redshift: MLCS  parameter~100 SDSS supernovae Ia in 2005 Which is real data and which is the simulation?Fewer fast decliners than expected - Over represented in Low-z sample? Selected against in SDSS color cut?Host Extinction vs Galaxy Type:SFR ~ Lu1.19 Hopkins et al. 2004SDSS u is a good measure of the SFR.SDSS z is a good measure of the number of stars in the galaxyu-z is then theSFR/star =the specific SFRu-z>4 may show lower dust extinction SN Luminosity vs Specific SFR:Bright AND faint SNIa happen in galaxies with SSFR u-z >2But only bright SNIa occur in u-z <1 Prompt SNIa have slow light curves - are brighter - make more 56NiHubble Residuals:~0.20 mag dispersion may be due to a “third” parameter (width and color are the first two)Projected Galacto- centric distance - expect high dispersion near center.Extinction - clear correlation due to Baysian prior in MLCSSpecific SFR - no correlation. So even in extreme SSFR hosts MLCS works.Host Color-Magnitude Diagram:Number of stars in the host versus Specific Star Formation Rate.Highest specific SFR hosts are also the smallest hosts.How do these hosts compare with field galaxies in the SDSS?15000 SDSS galaxies out to photo-z <0.35SNIa Host versus Galaxy/Stellar Frequency:SNIa host frequency versus field galaxy frequency => SNIa rate per galaxy.For u-z <2, the SNIa rate goes like the number of galaxies.Convert the relative number of galaxies to the relative number of stars by summing over the z absolute magnitudeFor u-z >4, the SNIa rate goes like the number of stars.Specific SNIa Rate versus Specific SFR:Divide the number of SNIa detected divided by the number of stars per SSFR bin.Normalize to the rate at the u-z =3 bin.Log (SNIa rate/star) goes as 0.9(u-z) for blue galaxies and is flat for red galaxies SN rate/star = 0.8+10-0.9(u-z)+2.3See:Mannucci et al. 2006Sullivan et al. 2006Scannapieco & Bildsen 2006Summary
  • SDSS-II SN Survey has good spectra and light curves for >100 SNIa
  • in 2005 and >300 in the first two years.
  • SDSS missing very fast decliners at z~0.1 to 0.2, or they aren’t there
  • SDSS finds only luminous SNIa in small, high SFR hosts: prompt
  • channel makes lots of 56Ni
  • No correlation between Hubble residuals and SSFR: good for cosmology.
  • Confirm the very high specific SNIa rate in high SSFR galaxies. See the
  • that the rate goes like the number of stars for red galaxies.
  • Preliminary results suggest no correlation between
  • host metallicity and SNIa peak brightness for early-type galaxies.
  • Preliminary results show a strong correlation between
  • peak SNIa brightness and population age in early hostsB. Dilday, U. Chicago
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