1 / 7

PILOT Survey for Supernovae in Starbursts

PILOT Survey for Supernovae in Starbursts. Stuart D. Ryder Anglo-Australian Observatory Seppo Mattila Stockholm Observatory. SN 2001ig (Ryder et al. 2004, MNRAS, in press). Why Supernovae?. Core-collapse SNe (CCSNe) generate/liberate the bulk of the light metals.

tobit
Download Presentation

PILOT Survey for Supernovae in Starbursts

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. PILOT Survey forSupernovae in Starbursts Stuart D. Ryder Anglo-Australian Observatory Seppo Mattila Stockholm Observatory

  2. SN 2001ig (Ryder et al. 2004, MNRAS, in press) Why Supernovae? • Core-collapse SNe (CCSNe) generate/liberate the bulk of the light metals. • CCSNe directly trace recent massive SFR (cf. UV, Ha, FIR, radio, [Fe II], …) • Can serve as probes of extinction and ISM. • CCSNe blast wave probes progenitor mass-loss history.

  3. Why Starbursts? • “Supernova Factories” – ULIRGs (LIR > 1012 L) have SFRs > 100 M yr -1, so > 1 CCSN yr -1. • High Z  high MLR, may influence SN evolution. • ULIRGs/starburst galaxy nuclei are crowded, heavily-extincted (AV > 10) regions  NIR, radio. • NIR allows follow-up at much earlier epochs; not all CCSNe are “radio-loud”. • WHT+INGRID/LIRIS K-band monitoring of 40 nearby (D < 45 Mpc) non-AGN starbursts. • VLT+NACO monitoring of 14 ULIRGs out to D ~ 300 Mpc.

  4. Historical SN in NGC 7714 • Found in archival UKIRT K image from Sep 1998. • Optimal Image Subtraction (Allard & Lupton 1998). • < 1 kpc from nucleus. • Not seen in U, J, H AV > 6.

  5. AO on ULIRGs • Require Strehl ratios ~0.2 – 0.3 to yield 0.06" (100 pc) resolution @ 300 Mpc. • NACO currently delivers (time variable) SR ~ 0.1 when guiding on ULIRG nucleus. NICMOS 1" IRAS 23128-5919 IRAS 17208-0014

  6. Discovery rate • Assume: • Stable, near diffraction-limited (0.3") PSF over FOV of InSb array (0.23" pix-1). • 10 min exposures  10s for K=22.5. • Monitor 15 ULIRGs out to 150 Mpc. • Detectable fraction increases with nuclear distance out to 500 pc. • M82 SNR extinction distribution (AV ~ 24, s ~ 9). • Template light curves for “ordinary” (MK ~ –18.6) and “slowly declining” (MK ~ –20.0) CCSNe.

  7. Summary • Expect: • 4–6 CCSNe (for 5–30% slow-decliners) by observing sample annually; • 9 CCSNe per year by observing each galaxy 3 times; • More frequent monitoring  light curves. • PILOT would deliver comparable CCSNe discovery rates to AO ULIRG survey on 8m, or nearby starburst survey with 4m telescopes.

More Related