List of objects for April, 23/24 and 24/25 observations
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object |
Type |
coordinates |
last mag |
comments |
Priority |
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from March, 5 targets list |
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SN 2009ao (disc. 2009/02/04.12)
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IIP |
16.6CR (Apr, 13.852) |
Spectra (range 402.7-1011 nm, Mar. 16.1-16.2): SN 2009ao is a young type-IIP supernova around a week past explosion; adopting a host-galaxy recession velocity of 3339 km/s (Chengalur et al. 1993, Ap.J. 419, 30) for the host galaxy (NGC 2939), H_beta is measured to be blue-shifted by roughly 8000 km/s. (CBET#1725)
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? |
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SN 2009ar = CSS090219:095526-012821 = 'css2' (discovered
2009/02/19)
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IIb |
09:55:25.71 -01:28:21.3 |
20.3R (Mar, 06.35) FAINT OBJECT! |
The presumed host galaxy to 2009ar, SDSS J095525.67-012821.0, has Gunn magnitudes u = 23.2, g = 21.7, r = 21.5, i = 21.6, z = 21.9. SN 2009ar is a type-IIb supernova at z = 0.026 and is most like SN 1996cb at one day past maximum (Feb, 25). |
? [OI], phase ~ 70 days. look 2008ApJ...687L...9M |
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SN 2009Z (disc 2009/02/02.53)
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II-pec? 1993J - like |
14:01:53.6 -01:20:30.2 |
17.25R (Mar, 25) |
Stritzinger, Morrell, and M. Phillips (also LCO) add that they have obtained spectra (range 403-1011.2 nm) of 2009Z (cf. CBET 1685) on Feb. 11.1 and 15.1 with the 6.5-m Magellan I (BAADE) telecope (+ IMACS). Cross- correlation with SNID shows these spectra to be most similar to those of SN 1993J at two days before and three days after maximum, respectively. |
? |
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deep field of GRB030226 |
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11:33:04.9 +25:53:55.6 |
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discovery of cosmological SNe using substracting of previously observed field of GRB030226 |
excluded |
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from April,3 targets list |
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SN 2009bw (discovered Mar, 27.871)
|
II |
03:56:06.92 +72:55:40.9 (low) |
14.8CR (Apr,16.863) |
from CBET#1746: but, in addition, H_alpha shows a narrow emission component at the host-galaxy redshift (1155 km/s; Schneider et al. 1992, Ap.J. Suppl. 81, 5) |
? to obtain the second our spectrum. |
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SN 2009ba (discovered Mar, 21.18)
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? |
09:59:01.92 +17:49:00.1(good; first part of night) |
March, 29: R~18.8 |
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? |
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SN 2009az (discovered Mar, 20.30; close to host nuclei)
|
I? |
10:55:56.22 +36:51:43.0(good, high; first part of night) |
faint, >19 |
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?, possibly no cause of close host nuclei |
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2009by (discovered Mar, 29.28)
|
II or IIn (CBET#1756) |
11:13:56.22+4:17:58.5 (good; first part of night) |
18.1R (April, 3) |
not observed in SAO yet! |
? |
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SN 2008in (disc. 2008 Dec, 26.79)
|
IIP |
12:22:01.77+04:28:47.5(normal altitude, first part of night) |
still bright |
observed on April, 3/4 |
? proposed by R.Roy |
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CSS090319:125916+271641 = 090319d = SN 2009cb (disc Mar, 19.408)
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? |
12:59:15.85 +27:16:41.3 (good, high) |
FAINT
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type determ. |
possibly, no |
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CSS090317:140750+363837=090317a = SN 2009bp (disc Mar, 17.50)
|
Ia |
14:07:49.75 +36:38:37.1 (good, high) |
>19
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A. Drake wrote: “I would avoid following Ia's like CSS090317:140750+363837 and CSS090319:142155+260102” |
?, all range spectrum, host spectrum |
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CSS090319:142155+260102=090319c = SN 2009db (disc Mar, 19.408)
|
Ia |
14:21:54.63 +26:01:02.0 (good, high) |
18.55R (Apr, 4)
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A. Drake wrote: “I would avoid following Ia's like CSS090317:140750+363837 and CSS090319:142155+260102” |
? all range spectrum, host magnitude |
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SN 2009bz (disc Mar, 29.48)
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II |
15:19:26.04 +11:03:30.1 (good; second part of night) |
16.9 (2009/03/29.48)
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? monitoring |
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CSS090319:152356-081918=090319b = SN 2009br (disc Mar, 19)
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? |
15:23:56.14 -08:19:18.3 (low) |
~19 (now)
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? type determ. |
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SN 2009ay (disc Mar, 20.41)
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II |
17:48:22.97 +54:08:54.7 (good; second part of night) |
15.8CR (Apr, 16.962) |
(standards by Tsvetkov, squares) |
? monitoring |
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will be observed by Stefano Benetti |
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SN 2009dc (disc Apr, 9) |
Ia |
15:51:12.12 +25:42:28.0 |
~16.5 |
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? Ia-type |
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SN 2009bw (see uper) |
II |
03:56:06.92 +72:55:40.9 (low, z=55) |
14.8CR (2009/04/16.863) |
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? |
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SN 2009cz (disc Apr, 6) |
Ia |
09:15:00.02 +29:44:07.1 |
~17.9 |
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? Ia-type |
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SN 2009dd |
II |
12:05:34.1 +50:32:19.4 (good, high) |
13.5 |
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? |
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SNe from Stefano Benetti's web-site http://web.oapd.inaf.it/supern/followup/ |
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SN 2009at (disc Mar, 11.633) |
II |
13:46:26.68 +46:06:09.1 (good, high) |
15.7C (2009/04/14.880) |
Stefano wrote about it's site at the letter |
? |
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SN 2009E (disc Jan 03; old) |
II |
12:09:49.56 +58:50:50.3 good, high; first half of night |
16.2CR (2009/04/16.984) |
Stefano wrote about it's site at the letter |
? |
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Newly discovered objects |
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2009dm (discovered Apr, 19.24)
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II or IIP near max. |
17.5C (Apr., 19.24)
corresponds with a SNID calculated z=0.024.The expansion velocity deduced from the H_alpha absorption is about 9200 km/s (Apr.,21.2) |
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? |
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2009dn (discovered Apr, 11) CLOSE TO NUCLEI
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? close to max |
11:37:39.33 +46:57:11.3 |
Apr., 7 >18.3C 17.5C (Apr., 11,12,14,15,16) 16.9C (Apr., 20.17) |
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? |
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SN 2009de (disc Jan, 2; old)
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Ic?
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13:00:37.49 +17:50:57.0
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19.5C (Apr, 19.2) |
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? |
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proposed by Andrew Drake |
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CSS090417:095440+191113 (disc Apr,17)
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?
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09:54:40 +19:11:13 |
r-i=0
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To avoid Ia's I would suggest not following anything with gunn colours r-i < -0.3 (A. Drake) |
? |
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CSS090418:081414+242340 (disc Apr,18)
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? |
08:14:14 +24:23:40 |
r-i=-0.26
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? |
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CSS090421:133609+340319 (disc Apr,21)
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? |
13:36:09 +34:03:19 |
r-i=?
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? |
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CSS080928:160837+041627 (discovered 2008/09/28)
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IIn |
16:08:37.23 +04:16:26.7 |
Mar, 21 17.6C
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Finally, as you may
have seen in our recent ATel, |
? |
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also look at non-classif. SN-candidates at http://nesssi.cacr.caltech.edu/catalina/AllSN.html
K. Konishi, Y. Ihara, and K. Tokita, University of Tokyo; N. Morimoto,
Tohoku University; and T. Hattori, National Astronomical Observatory of Japan,
report that a spectrogram (range 370-900 nm) of 2009by (cf. CBET 1748),
obtained on Apr. 4.28 UT with the 8.2-m SUBARU Telescope (+ FOCAS), shows it
to be a type-II supernova. Their recently-developed identification code
suggests that the spectrum is best fitted to that of the type-IIP supernova
1999em at five days after the explosion (Elmhamdi et al. 2003, MNRAS 338,
938). There are narrow emission-line components of H_alpha and H_beta,
corresponding to z = 0.021 +/- 0.001; it is unclear whether these narrow
components originate from the H II region of the host galaxy or are intrinsic
to the supernova. Thus, it the possibility cannot be excluded that this
supernova is of type IIn.
NOTE: These 'Central Bureau Electronic Telegrams' are sometimes
superseded by text appearing later in the printed IAU Circulars.
2009 April 6 (CBET 1756) Daniel W. E. Green
all coordinates:
09bw 03:56:06.92 +72:55:40.9
09ba 09:59:01.92 +17:49:00.1
09az 10:55:56.22 +36:51:43.0
09by 11:13:56.22 +4:17:58.5
08gz 11:25:03.24 -09:47:51.0
08in 12:22:01.77 +04:28:47.5
09cb 12:59:15.85 27:16:41.3
17a 14:07:49.75 36:38:37.1
19c 14:21:54.63 26:01:02.0
09bz 15:19:26.04 +11:03:30.1
19b 15:23:56.14 -08:19:18.3
09ay 17:48:22.97 +54:08:54.7
09dc 15:51:12.12 +25:42:28.0
09cz 09:15:00.02 +29:44:07.1
09dd 12:05:34.1 +50:32:19.4
09at 3:46:26.68 +46:06:09.1
09E 12:09:49.56 +58:50:50.3
09dm 11:30:20.14 +44:09:49.2
09dn 11:37:39.33 +46:57:11.3
09de 13:00:37.49 +17:50:57.0
0417 09:54:40 +19:11:13
0418 08:14:14 +24:23:40
0421 13:36:09 +34:03:19
0928 16:08:37.23 +04:16:26.7
Unusual CRTS Transient
ATel #1768; A.J.
Drake, A. Mahabal, S.G. Djorgovski, R. Williams, M.J. Graham (Caltech); E.C.
Beshore, S.M. Larson (LPL; M. Catelan (PUC); E. Christensen (Gemini
Observatory); E. Christensen (Gemini Observatory); E.C. Beshore, S.M. Larson
(LPL/UA)
on 7 Oct 2008; 23:51 UT
Password Certification: Andrew J. Drake (ajd@cacr.caltech.edu)
Subjects: Optical, Request for Observations,
Transients, Variables
Referred to by ATel #: 2010
We have detected an optical transient of unknown nature in Catalina 0.7m Schmidt telescope images from 28 Sep 2008 UT. The object has the following parameters:
|
2008-09-28 UT 02:50:49 |
RA 16:08:37.23 |
Dec 04:16:26.7 |
Mag 17.7 |
Type ? |
A possible uncataloged match to the transient is present in SDSS images with magnitude r~22.5. The transient is visible in Catalina images dating back to Sep 13th 2007 and is gradually brightening suggesting the transient may be distant, high amplitude (~5 mags), long period variable. However, the object is not seen in archival DSS1 and DSS2, 2MASS, or PQ images covering this location. Furthermore, follow-up photometry taken with the Palomar 60" telescope on Sep. 29.12 UT gives g=18.3, g-r=1.0, r-i=-0.5 and g=18.1, g-r=0.7, r-i=-0.32 on Oct 10.12. The r-i colours fall far from the stellar locus and the colours expected for long period variables. Further follow-up is requested.
For
finding charts and discovery images please see:
http://voeventnet.cacr.caltech.edu/feeds/ATEL/CRTS.
CRTS optical transients are detected and published as VOEvents in real-time at
http://voeventnet.org/feeds/Catalina.shtml and in RSS here
http://voeventnet.caltech.edu/feeds/Catfeed.xml
CRTS Discovery of a very energetic Type IIn Supernova
ATel #2010; A..A. Mahabal, A.J. Drake, S.G. Djorgovski, M.J. Graham, R.
Williams, W. Max-Moerbeck (Caltech); M. Catelan (PUC, Chile); E.C. Beshore,
S.M. Larson, A. Gibbs, R. Kowalski, A. Boattini, R. Hill (LPL/UA); E.
Christensen (Gemini Observatory); V. Mohan, A.N. Ramaprakash, A.K. Kembhavi
(IUCAA);
on 10 Apr 2009; 22:45 UT
Distributed as an Instant Email Notice (Request for Observations)
Password Certification: Ashish Mahabal (aam@astro.caltech.edu)
Subjects: Optical, Novae, Supernovae, Transients
The Catalina Real-time Transient Survey (CRTS) has spectroscopically characterized CSS080928:160837+041626 (ATel 1768) as a Type IIn SN at z~0.041 using the SMARTS 1.5m telescope using Observations taken on March 27th UT with the following results:
|
ID |
RA |
Dec |
Type |
z |
Disc. ATel |
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16:08:37.23 |
04:16:26.7 |
IIn |
0.041 |
ATEL#1768 |
The object was first marked as a transient by CRTS on 2008-09-28 (unfiltered mag=17.7). It was also present in the 2007-09-13 images, but blended with the brighter star nearby and hence not detected as a transient. Palomar-Quest images from 2007-02-24 do not reveal the presence of the SN. GALEX data from 2008-06-05 shows a well-detected source at this location (NUV 19.93+/-0.04, FUV 21.18+/-0.09). It was not seen in AIS images from 2004-05-17 indicating a brightening in NUV by at least 2.5 mags. Coadded images from SDSS (all filters) reveal the presence of a possible faint host at the location. Assuming that the galaxy has r=23, at z=0.041 it translates to M_r=~-13, almost a 100 times dimmer than the LMC.
Palomar 60-inch (P60) data form 2009-03-21 reveals that it is still bright (r=17.60+/-0.04). It has stayed bright for over 500 days, and rising much of the time. In fact the SMARTS spectrum with its Balmer lines (strong H-alpha, H-beta, H-gamma), He I lines (5876, 7065 and possibly others), and an absence of Oxygen lines reveals it to be much more like SN1994Y at T=30 days (Filipenko A.V., ARAA, 1997, 35, 309-355, Fig. 14). There is also some evidence of Fe-I emission and the H-beta shows a P-Cygni like profile. The maximum P60 r-band magnitude was ~17.2 suggesting an absolute magnitude ~-18.8. The evidence is consistent with a type IIn supernova possibly with high density circumstellar material.
Additional observations are requested.
All current candidate and confirmed SNe as well as finding charts can be found here.