Supernovae: from Stellar Evolution to Cosmology
Massimo Turatto – Padova - Italia Outlook
• Lesson a – Introduction to SNe • Lesson b – SN 1987A in LMC
• Lesson c – SN general properties • Lesson d – SN progenitors and models
• Lesson e – Thermonuclear SNe
• Lesson f – Core Collapse SNe
• Lesson g – SN rates • Lesson h – SNe and Cosmology • Lesson i – SNe and GRB Lesson a
Introduction to Supernovae
1.History
2.Discovery techniques
3.Numerology Definition of Supernova
Explosive event disrupting a star at the end of its (single or binary) evolution, returning to the Inter-Stellar Medium all (or most) the gas synthetized during its evolution and explosion. Kepler SN 1604 De Stella Nova in Pede Serpentarii
Galileo: no significant parallax Î above the Moon against Aristotle’s Cosmology (Digges already for SN 1572) .. generated by the embrace of Mars and Jupiter at the time of their encounter
Novae and Supernovae
• Novae observed since millennia in the East and in the West • Few in “Nebulae” (S And 1885)
• Lundmark (1919) Î D(And)=200Kpc Î MSN1885=-15 • Lundmark (1925) Î “It is quite possible that we have to deal with two distinct classes of Novae: one 'upper class' having comparatively few members and reaching an absolute magnitude more or less equal to the absolute magnitude of the system in which they appear: one 'lower class' in the mean 10 magnitudes fainter ...”
• Baade & Zwicky 1933-1934 Î SuperNovae as final stages of Stellar Evolution, sources of cosmic rays and result of creation of NS (!!) Historical SNe (Stephenson & Green 2005) • Investigations of ancient (East and West) chronicles
Criteria: 1. Long duration of visibility 2. Fixed location 3. Low b 4. No angular extent 5. Unusual brilliance 6. Independent records 7. (association with SNR) “safe” historical supernovae only 8 reliable events: Year Date Con RA Dec mag Comment/SNR • 185 AD Cen 14:43.1 -62:28 -2(-6??) SNR: G135.4-2.3/RCW 86 • 386 Sgr SNR: G11.2-0.3 (?) • 393/396 Sco 17:14 -39.8 -3 3 radio sources candidates for SNR • 1006 Apr 30 Lup 15:02.8 -41:57 -9(+-1) SNR: PKS 1459-41 • 1054 Jul 4 Tau 05:34.5 +22:01 -6 M1 Crab Nebula • 1181 Aug 6 Cas 02:05.6 +64:49 -1 3C 58 • 1572 Nov 6 Cas 00:25.3 +64:09 -4 Tycho • 1604 Oct 9 Oph 17:30.6 -21:29 -3 Kepler • 1680? 1667? Cas 23:23.4 +58:50 6? Cas A SN
(Stephenson & Green 2005; http://www.seds.org/messier/more/mw_sn.html)
SN discovery (SN 1998S) Image to be searched Reference image Subtracted image
SN 2000fc type Ia V=22.4 z=0.42 IAUC7537 Each image is the sum of three 15min exposures
The search is based on the comparison of two images taken at different epochs. The image with the best seeing is matched to the other and the reference frame is subtracted using ISIS2.1 package. The difference image is searched for candidates using sextractor. Then we use a scoring algorithm tuned after artificial star experiment to sort the candidates. Early searches
• 1885: a bright nova is discovered in the Andromeda Nebula • 1936: Zwicky systematic SN search using the new 18 inch Schmidt telescope • 1941: Minkowski provisionally divides SNe in type I and II Palomar 18 inch Schmidt telescope Field of view 9 x 9 deg limit discovery magnitude 16.5
Monitoring 150 nebular fields covering 1/5 of the entire sky visible from Palomar.
Sept.1936 -- 1941 19 SNe 1 SN / 135 photographs 1 SN / 8 nights exposure time 1936-1938: 3 SNe First estimate of the Palomar 18 inch SN rate 1/ 600yr /galaxy Zwicky, F. 1938, ApJ 88,529
1936-1941: 19 SNe - Control time method -SN rate 1/ 359yr /galaxy - independent on galaxy type Zwicky, F. 1942, ApJ 96,28 The golden age
• 1957: Schmidt telescopes devoted to SN searches in Zimmerwald (CH, P. Wild), Asiago (I, L. Rosino), Tonantzintla (MX, G. Haro, E. Chavira) • 1958: Palomar 48-inch Schmidt telescope began SN search • 1961: Coordinated international SN search • 1968: First SN by an amateur (J. Bennet SN 1968L) Asiago 40/50cm Schmidt telescope (1958 -1992)
Field of view 5.5 x 5.5 deg Limit discovery mag 16.0 Asiago 67/92 cm Schmidt telescope (1966 Æ )
Field of view 5.5 x 5.5 deg Limit discovery mag 17.0 1954A Zwicky international end of Palomar Palomar SN search 48 inch search 1972E Asiago 40/50 Schmidt The modern times
• 1975: “Zwicky” Palomar SN search ends • 1979: Southern SN search (Maza) • 1980: Evans begins his visual SN search (43 SNe) • 1981 CCD automated SN search • 1986 High redshift SN search z=0.2-0.4 • 1987 in LMC the brightest SN in the last 4 centuries MT graduates with a thesis on SNe
Ωλ>0 1998bw 1988T GRBs z = 0.28 1995at z = 0.66 end of Palomar Southern search SN 1987A searches Today
• LOTOSS 251; LOSS 139 • BAOSS 41 •QUEST 62 •EROS 60 • MSACSST 50 • + amateurs astronomers Sky distribution of SNe discovered to date Equatorial coordinates <1980 511 SNe 1980-1998 944 SNe >=1999 1295 SNe SN distribution in galactic coordinates Sky coverage of SN searches <1980 >=2002 z < 0.01 z > 0.1 Galaxy types Distribution of SN magnitudes SN redshift distribution
LOTOSS SNe & spiral galaxy inclination Di Paola et al. (2002) A&A393, L21
II+Ib/c AV>6 mag 2002cv Sb-Scd
Ia
S0-Sab
2002bo AV =1.5 mag Iband SN types vs. galaxy types SN Numerology
• Asiago supernova Catalogue (Barbon et al. 1984, 1989, 1999) • http://web.pd.astro.it/supern/snean.txt
pec 2% (20/6/2005) Ibc 1% • Tot SNe 3154 Ic 3% Ib 1%
-- 32% II 23%
I 3%
Ia 35% SN 1987A SN 1998bw • (too) large number of SN types • SNIa also in E • No SNII, Ib/c in early type galaxies • Different distribution among types High-z SN searches mid ’80s: • Danish 1.5m (Norgaard-Nielsen et al.) in the ’90s: •SCP (Perlmutter et al.) • High-z SN Search (Schmidt et al.)
Î ΩΛ=0.7 in the ’00s: • Essence (Tololo, Smith et al.) • Legacy Survey CFHT (PI-less) Î w=p/ρ Southern Intermediate Redshift ESO SN Search (aimed to the SN rates) [email protected] Effective search area ~5.1 Telescope aperture: 2.2 m square degrees Field of view: 34`x 33` Spectroscopic follow up with Pixel scale: 0.238 arcsec/pix VLT+FORS1/2
12(+13) nights ESO 2.2+WFI 6 nights VLT
• 21 fields • > 500 Gby of raw data • > 500 science exposures • > 100 candidates SN search
target reference difference - =
SN 2000fc type Ia z = 0.42 V=22.4 IAUC7537 SouthernSSouthern InIntermediatetermediate RRedshiftedshift E ESOSO SSNN SearchSearch 1. Observations: ESO2.2+WFI 2. SN search: STRESS package • Data reduction Æ mscred • Image subtraction Æ ISIS2.1 • Candidate detection Æ sextractor + “score” 3. SN confirmation • Spectroscopy (VLT+FORS) • Photometric history (mysql database) 4. Estimate of the detection efficiency • Artificial star experiment • Control time 5. Characterization of the galaxy sample: • Deep stacked images Æ swarp • Photometric redshift Æ hyperz 6. Compute the rate SN Searches
SN 2001gf Ia z=0.132 SN2001gj II z = 0.27 ≈30% of candidates turn out to be AGNs. 34 spectroscopically confirmed SNe Ia cc
Ia/All = 45% VLT Survey Telescope + OmegaCAM
location: Paranal (Chile) size: 2.6 m field of view: 1 x 1 deg
Large Binocular Telescope + LBCs
location: Mt. Graham (Arizona) size: 2 x 8.2 m field of view: 23 x 23 arcmin
25% of the observing time for the Italian community