IAU Circulars (IAUCs) - циркуляры МАС - 08/2010

[Tikhon]

3 August 2010
IAU Electronic Telegram No.2397

SUPERNOVA 2010gs IN PGC 65331

Further to CBET 2389, on behalf of the "La Sagra Sky Survey" (LSSS)
Supernova Search Team (which includes also Denis Vida, Ivica Skokic, Robert
Gregic, David Gostinski, Salvador Sanchez, Jaime Nomen, Reiner Stoss, Bill
Yeung, Juan Rodriguez, and Miguel Hurtado), Filip Novoselnik reports the
discovery of an apparent supernova (mag 16.6) on three CCD images (limiting
mag about 20.0) taken on Aug. 1.876, 1.888, and 1.900 UT with a 0.45-m
telescope. The new object, which was confirmed at V = 17.6 on three stacked
90-s exposures taken with a 0.40-m telescope at Observatorio Astronomico de
La Sagra on Aug. 2.987, is located at R.A. = 20h45m39s.51 +/- 0s.01, Decl. =
-5d35'11".8 +/- 0".8 (equinox 2000.0), which is 5" west and 10" north of the
nucleus of the galaxy PGC 65331. Nothing is visible at this position on a
Digitized Sky Survey image from 1985 July 11 (limiting red mag 22) or on a
Sloan Digital Sky Survey image from 2000 Sept. 3 (limiting I mag 23). An
image of 2010gs has been posted by Novoselnik at the following website URL:
http://img838.imageshack.us/img838/5093/sncandcrop.jpg.

NOTE: These 'Central Bureau Electronic Telegrams' are sometimes
superseded by text appearing later in the printed IAU Circulars.

2010 August 3 (CBET 2397) Daniel W. E. Green

[Tikhon]

3 August 2010
IAU Electronic Telegram No.2398

NO NOVA IN M32 (M32N 2010-07a)

Kamil Hornoch, Astronomical Institute, Ondrejov; Ondrej Pejcha, and
Robert F. Wing, Department of Astronomy, Ohio State University; Ovidiu
Vaduvescu and Andrew Cardwell, Isaac Newton Group of Telescopes; and Jose L.
Prieto, Carnegie Observatories, report their results of photometry and
spectroscopy of the presumed nova announced on CBET 2379. In view of the
apparent red color of the object and lack of strong H_alpha emission (see
photometric measurements below), Vaduvescu and Cardwell obtained a low-
resolution optical spectrum (range 350-900 nm, resolution 1.3 nm) with the
4.2-m William Herschel Telescope (+ ACAM) at La Palma on July 23.15 UT. The
spectrum shows TiO absorption bands consistent with an M2 star. The
luminosity-sensitive features at rest wavelength 649.7 nm and a broad CN
absorption at 795 nm are present, and their strengths suggest a supergiant
luminosity. There is a narrow (consistent with instrumental profile) and
weak H_alpha emission with equivalent width 0.46 nm. The radial velocity
of H_alpha emission is -290 +/- 40 km/s, which favors membership in M31
but does not disprove membership in M32. The implied absolute magnitude is
about M_R = -4.7.
In addition, they found that M32N 2010-07a is possibly associated with
a rather red object in the catalogue of variable stars from the POINT-AGAPE
survey (An et al. 2004, MNRAS, 351, 1017). The object with number 95143 has
a period of 258 days and is located at R.A. = 0h42m32s.515, Decl. =
+40o53'36".783 (equinox 2000.0), which is 0".7 east and 0".1 south from the
best position of M32N 2010-07a obtained from the recent images taken by D.
Pinfield, B. Sipocz, and G. Kovacs with the 2.54-m Isaac Newton Telescope
(+ WFC) at La Palma. Based on the available evidence, they propose that
M32N 2010-07a is a long-period variable star currently slowly declining
from maximum brightness.
The following additional magnitudes of M32N 2010-07a were measured by
Hornoch from available images: 2010 July 19.186 UT, Sloan r' = 20.20 +/-
0.06 (Pinfield, Sipocz, and Kovacs, 2.54-m Isaac Newton Telescope at La
Palma); 19.191, [H_alpha] = 19.9 +/- 0.15 (Pinfield, Sipocz, and Kovacs);
20.121, [H_alpha] = 19.8 +/- 0.15 (J. Gorosabel, O. Lara Gil, M. Jelinek,
P. Kubanek, and P. Martorell, 1.23-m telescope at Calar Alto); 21.934, R-I
= +0.9 +/- 0.3 (Hornoch and P. Zasche, 0.65-m telescope at Ondrejov);
23.175, Sloan g' = 21.7 +/- 0.2 (Vaduvescu and Cardwell, 4.2-m William
Herschel Telescope at La Palma); 23.177, Sloan r' = 20.29 +/- 0.05
(Vaduvescu and Cardwell); 23.180, Sloan i' = 19.35 +/- 0.02 (Vaduvescu and
Cardwell).

NOTE: These 'Central Bureau Electronic Telegrams' are sometimes
superseded by text appearing later in the printed IAU Circulars.

2010 August 3 (CBET 2398) Daniel W. E. Green

[Tikhon]

3 August 2010
IAU Electronic Telegram No.2399

SUPERNOVA 2010gt IN ESO 187-21

L. A. G. Monard, Pretoria, South Africa, reports his discovery of an
apparent supernova (magnitude about 18.0) on several unfiltered CCD images
taken on Aug. 2.867 UT at the Bronberg Observatory. The new object, which
was confirmed at magnitude about 17.7 on Aug 3.806, is located at R.A. =
20h51m22s.38, Decl. = -52d32'48".1 (equinox 2000.0), which is 3" east and
11" north of the galaxy core of ESO 187-21. Nothing is shown at the position
in Digitized Sky Survey images down to red mag 20.5 or on the previous image
of this galaxy taken at the Bronberg Observatory on 2010 July 7.067 (limiting
mag 19.0) or on earlier images from there.

NOTE: These 'Central Bureau Electronic Telegrams' are sometimes
superseded by text appearing later in the printed IAU Circulars.

2010 August 3 (CBET 2399) Daniel W. E. Green

[Tikhon]

4 August 2010
IAU Electronic Telegram No.2400

COMET P/1999 XB69 = 2010 C2 (LINEAR)

G. V. Williams, Minor Planet Center, has identified comet P/1999 XB69
in WISE data:

2010 UT R.A. (2000) Decl. Mag.
Feb. 1.56490 14 30 58.74 -25 34 02.2 21

He subsequently identified the comet in data from the Mount Lemmon Survey
on 2008 Oct. 31. The indicated correction to the prediction on MPC 56804
is Delta_T = -0.34 day.

Further details are given on MPEC 2010-P21.

NOTE: These 'Central Bureau Electronic Telegrams' are sometimes
superseded by text appearing later in the printed IAU Circulars.

2010 August 4 (CBET 2400) Brian G. Marsden

[Tikhon]

4 August 2010
IAU Electronic Telegram No.2401

2010 PERSEID METEORS

P. Jenniskens, SETI Institute; and J. Vaubaillon, Institut de Mecanique
Celeste et de Calcul des Ephemerides, Paris, report that the annual Perseid
shower (IAU Shower 7) is expected to peak with a broad maximum around Aug.
13d03h20m UT (solar longitude 140.14 deg, equinox 2000.0), with best viewing
conditions in Europe in the early morning hours, while numerous long trails
will be visibile in the early evening hours in (eastern) North America. In
addition, a brief 1-hour period of elevated rates can occur from an encounter
with dust ejected by comet 109P/Swift-Tuttle in 1479. Current models put
this dust trail just outside of the earth's orbit. The peak time is
predicted for Aug. 12d16h49m UT (solar longitude 139.7292 deg), which is an
update from Jenniskens (2006, *Meteor Showers and their Parent Comets*, p.
657).

NOTE: These 'Central Bureau Electronic Telegrams' are sometimes
superseded by text appearing later in the printed IAU Circulars.

2010 August 4 (CBET 2401) Daniel W. E. Green

[Tikhon]

6 August 2010
IAU Electronic Telegram No.2402

(8026) 1991 JA_1

B. D. Warner, Palmer Divide Observatory and MoreData, Colorado Springs,
CO, U.S.A.; and Alan W. Harris, MoreData, La Canada, CA, report that
photometric observations obtained during July 11-17 reveal that minor planet
(8026) may be an unusual binary system. There is a well-defined period of
2.300 +/- 0.001 hr and amplitude of 0.12 mag, typical of many asynchronous
binary systems. They find another period of about 320 hr with an amplitude
(A) of about 0.40 mag, distinctly atypical of such systems.
This system may represent a new type of binary system -- where the
primary has a very long period and a satellite with a short period -- that is
not tidally locked to the orbital period. Similar traits were discovered for
minor planet (218144) 2002 RL_66 (Warner et al. 2010, Minor Planet Bulletin
37, 109-111), which had a primary period of 588 hr (A = 0.25 mag) and secondary
period of 2.49 hr (A = 0.04 mag). Neither system reveals an orbit period
through mutual eclipse/occultation events, suggesting that the orbit period
may be very long and the component separation large.
The authors request additional observations of (8026), including adaptive-
optic observations if possible, since there is a possibility of this being a
widely-separated pair. Photometric lightcurve data will need to be well-
calibrated on an internal (if not standard) photometric system in order to
link night-to-night brightness levels. The authors also ask any observers who
wish to participate to contact them (via brian@MinorPlanetObserver.com) to
arrange for coordination of observation and combined analysis of results.

NOTE: These 'Central Bureau Electronic Telegrams' are sometimes
superseded by text appearing later in the printed IAU Circulars.

2010 August 6 (CBET 2402) Daniel W. E. Green

[Tikhon]

11 August 2010
IAU Electronic Telegram No.2403

SUPERNOVAE 2010gs AND 2010gj

N. B. Andreasen, S. J. Jakobsen, and C. Heje Groenbech, DARS Summer
School -- together with J. Fynbo and J. Sollerman, Dark Cosmology Center,
Niels Bohr Institute, Copenhagen University -- report on optical spectroscopy
of SNe 2010gs and 2010gj obtained with the Nordic Optical Telescope (+ ALFOSC;
range 350-900 nm, resolution 0.8 nm) on Aug. 10.1 UT. The fully reduced
spectrum of 2010gs (cf. CBET 2397) in PGS 65331 shows this to be a fairly
young type-II supernova with clear Balmer-line P-Cyg profiles. SN 2010gj (cf.
2381) in PGC 190539 is instead a type-Ia supernova a month past explosion;
cross-correlation with the library of supernova spectra in SNID (Blondin and
Tonry 2007, Ap.J. 666, 1024), gives the best match for 2010gj with the
peculiar supernova 2005hk.

NOTE: These 'Central Bureau Electronic Telegrams' are sometimes
superseded by text appearing later in the printed IAU Circulars.

2010 August 11 (CBET 2403) Daniel W. E. Green

[Tikhon]

11 August 2010
IAU Electronic Telegram No.2404

POSSIBLE SUPERNOVA IN GALAXY IN DRACO

S. Nakano, Sumoto, Japan, reports the discovery by Koichi Itagaki
(Teppo-cho, Yamagata) of an apparent supernova (mag 16.4) on unfiltered
CCD frames (limiting magnitude 19.0) taken on Aug. 9.705 UT using a 0.60-m
f/5.7 reflector (+ Bitran BT-214E camera). The new object is located at
R.A. = 17h58m22s.56 +/- 0s.02, Decl. = +50o47'34".0 +/- 0".4 (equinox
2000.0), near a small and faint galaxy. Toru Yusa (Osaki, Japan) reports
his confirming images (limiting mag 18-19) of the new object taken remotely
at the RAS Observatory near Mayhill, NM, U.S.A., on Aug. 10.148 and 10.169,
providing position end figures 22s.56 +/0 0s.01, 34".6 +/- 0".1. Additional
unfiltered CCD magnitudes for the variable, including pre-discovery images
found by Itagaki from his archive: 2008 Aug. 31.50, [19.5 (Itagaki); 2010
Aug. 3.614, 17.5 (Itagaki); 6.576, 16.9 (Itagaki); 10.148, 16.0 (Yusa,
0.30-m f/12 reflector + FLI IMG1024-DM camera); 10.169, 16.0 (Yusa, 0.25-m
f/3.4 reflector + SBIG ST-10XME camera); 10.446, 16.2 (Itagaki); 10.527,
16.3 (Yusa, 0.30-m f/12 Cassegrain reflector + SBIG STL-1001E camera at
Osaki, Japan). Itagaki's pre- and discovery images of the new variable are
posted at website URL http://www.k-itagaki.jp/images/psn-anon-2.jpg. Also,
Yusa has posted an image of the variable at the following website URL:
http://www.palette.furukawa.miyagi.jp/s ... 100810.jpg. The
faint presumed host galaxy is SDSS J175822.33+504733.1.
Following posting on the Central Bureau's unconfirmed-objects webpage,
Vitali Nevski (Vitebsk, Belarus) writes that he obtained CCD images on Aug.
10.880 with a 0.3-m reflector that yield magnitude 15.8 and position end
figures 22s.58, 34".7 (USNO-B1.0 catalogue) for the possible supernova,
adding that nothing is visible at this position on a Palomar Sky Survey
image obtained on 1993 Aug. 16 (via the Digitized Sky Survey; limiting red
mag 21).

NOTE: These 'Central Bureau Electronic Telegrams' are sometimes
superseded by text appearing later in the printed IAU Circulars.

2010 August 11 (CBET 2404) Daniel W. E. Green

[Tikhon]

11 August 2010
IAU Electronic Telegram No.2405

SUPERNOVAE 2010gl AND 2010gr

I. K. W. Kleiser, J. M. Silverman, D. Poznanski, and A. V. Filippenko,
University of California, Berkeley, report that inspection of CCD spectra
(range 340-1000 nm), obtained on Aug. 10 UT with the 3-m Shane reflector (+
Kast) at Lick Observatory, shows that 2010gl (CBET 2382) is a type-Ia
supernova; after removal of the host-galaxy recession velocity of 5500 km/s,
determined from narrow absorption features, the absorption minimum of the
Si II 635.5-nm line is found to be blueshifted by about 10400 km/s.
Cross-correlation with a library of supernova spectra using the "SuperNova
IDentification" code (SNID; Blondin and Tonry 2007, Ap.J. 666, 1024) indicates
that 2010gl is about one week past maximum brightness. SN 2010gr (CBET 2396)
is a type-Ib/c (probably Ic) supernova, 1-3 months past maximum brightness.
S. Nakano (Sumoto, Japan) forwards a report from a Japanese amateur
named Nobuhisa Kojima who independently discovered 2010gl on July 21.67 UT at
mag 16.0; evidently unaware of the discovery report on CBET 2382, Koichi
Itagaki (Teppo-cho, Yamagata) confirmed 2010gl at mag 16.0 on July 23.57.
Subsequently, Kojima contacted Nakano to report that his unfiltered CCD
image taken on Aug. 6.65 shows 2010gl still bright at mag 15.8, using a
0.25-cm f/6.3 Schmidt-Cassegrain (+ Bitran BJ-41L camera).

NOTE: These 'Central Bureau Electronic Telegrams' are sometimes
superseded by text appearing later in the printed IAU Circulars.

2010 August 11 (CBET 2405) Daniel W. E. Green

[Tikhon]

11 August 2010
IAU Electronic Telegram No.2406

SUPERNOVA 2010gq IN PGC 1142

N. B. Andreasen, S. J. Jakobsen, and C. Heje Groenbech, DARS Summer
School -- together with J. Fynbo and J. Sollerman, Dark Cosmology Center,
Niels Bohr Institute, Copenhagen University -- report on optical
spectroscopy of SN 2010gq obtained with the Nordic Optical Telescope (+
ALFOSC; range 350-900 nm, resolution 0.8 nm) on Aug. 11.2 UT. The fully
reduced spectrum of 2010gq (cf. CBET 2389) in CGCG 382-041 shows this to
be a type-II supernova several months past explosion. The H-alpha line
has a FWHM of about 7500 km/s.

NOTE: These 'Central Bureau Electronic Telegrams' are sometimes
superseded by text appearing later in the printed IAU Circulars.

2010 August 11 (CBET 2406) Daniel W. E. Green

[Tikhon]

11 August 2010
IAU Electronic Telegram No.2407

SUPERNOVA 2010gu

Further to CBET 2387, R. H. McNaught and G. Garradd, Australian National
University; A. J. Drake, S. G. Djorgovski, A. Mahabal, M. J. Graham, and R.
Williams, California Institute of Technology; J. L. Prieto, Carnegie
Observatories; M. Catelan, Pontificia Universidad Catolica de Chile; E. C.
Beshore and S. M. Larson, Lunar and Planetary Laboratory, University of
Arizona; and E. Christensen, Gemini Observatory, report the CRTS discovery
of an apparent supernova in unfiltered Siding Spring Survey (SSS) images:

SN 2010 UT R.A. (2000.0) Decl. Mag. Offset
2010gu Aug. 7.67 22 19 23.16 -36 58 24.5 18.0 7".0 E, 3".3 N

Further SSS magnitudes for 2010gu: July 9.81, [19.5; Aug. 10.76, 17.9.
The host galaxy, 2MASX J22192259-3658278, has redshift z = 0.056.

NOTE: These 'Central Bureau Electronic Telegrams' are sometimes
superseded by text appearing later in the printed IAU Circulars.

2010 August 11 (CBET 2407) Daniel W. E. Green

[Tikhon]

12 August 2010
IAU Electronic Telegram No.2408

SUPERNOVA 2010gv

J. Sollerman and J. Fynbo, Dark Cosmology Center, Niels Bohr Institute,
Copenhagen University, on behalf of N. B. Andreasen, S. J. Jakobsen, and C.
Heje Groenbech, DARS Summer School, report on optical spectroscopy of the
possible supernova near a faint galaxy in Draco that was announced on CBET
2404. The spectroscopy was obtained with the Nordic Optical Telescope (+
ALFOSC; range 350-900 nm, resolution 0.8 nm) on Aug. 11.9 UT. The fully
reduced spectrum shows this object to be a young type-Ia supernova at, or
slightly before, maximum light.

NOTE: These 'Central Bureau Electronic Telegrams' are sometimes
superseded by text appearing later in the printed IAU Circulars.

2010 August 12 (CBET 2408) Daniel W. E. Green

[Tikhon]

12 August 2010
IAU Electronic Telegram No.2409

SUPERNOVA 2010gm IN MCG +07-36-25

J. Fynbo and J. Sollerman, Dark Cosmology Center, Niels Bohr Institute,
Copenhagen University, on behalf of N. B. Andreasen, S. J. Jakobsen, and C.
Heje Groenbech, DARS Summer School, report on optical spectroscopy of 2010gm
(cf. CBET 2383) obtained with the Nordic Optical Telescope (+ ALFOSC; range
350-900 nm, resolution 0.8 nm) on Aug. 11.9 UT. The fully reduced spectrum
shows 2010gm to be a normal type-Ia supernova slightly more than a month past
maximum light.

NOTE: These 'Central Bureau Electronic Telegrams' are sometimes
superseded by text appearing later in the printed IAU Circulars.

2010 August 12 (CBET 2409) Daniel W. E. Green

[Tikhon]

13 August 2010
IAU Electronic Telegram No.2410

SUPERNOVA 2010gw IN IC 4992

Peter Marples, Loganholme, Queensland, Australia, reports the discovery
of an apparent supernova (red mag 16.6) on a 35-s unfiltered CCD image taken
on Aug. 10.61 UT with a 35-cm Celestron C14 reflector (+ SBIG ST10 camera) by
Stuart Parker (Oxford, Canterbury, New Zealand) as a member of the Backyard
Observatory Supernova Search team. The new object is located at R.A. =
20h23m25s.31, Decl. = -71d34'04".9 (equinox 2000.0), which is 12" west and
11" south of the nucleus of IC 4992 (position and magnitude measured by
Colin Drescher and Greg Bock from the Queensland Astrofest, Camp Duckadang,
Linville, Queensland, Australia, using Astrometrica with the USNO-B1.0
catalogue). A confirming image taken on Aug. 12.371 by Bock using a Meade
35-cm f/7 reflector (+ ST10 CCD camera; limiting red mag 17.7) shows the
new object clearly, with nothing visible at the position of 2010gw on a
Digitized Sky Survey image (limiting red mag > 19).

NOTE: These 'Central Bureau Electronic Telegrams' are sometimes
superseded by text appearing later in the printed IAU Circulars.

2010 August 13 (CBET 2410) Daniel W. E. Green

[Tikhon]

13 August 2010
IAU Electronic Telegram No.2411

APPARENT NOVAE IN M31

Kamil Hornoch, Astronomical Institute, Ondrejov; and Jesus M. Corral-
Santana and Jorge Casares, Instituto de Astrofisica de Canarias and
Universidad de La Laguna, report their discovery of a probable nova in the
galaxy M31 on co-added 720-s narrow-band H_alpha and 360-s Sloan r' CCD
frames taken by Corral-Santana and Casares with the 2.54-m Isaac Newton
Telescope (+ WFC) at La Palma on July 10.210 and 10.200 UT, respectively.
The new object, designated M31N 2010-07b, is visible on single images used
for the co-added frame and is faintly visible also on many pre-discovery
co-added frames taken during June, but it is not present on numerous archival
images taken at Ondrejov and other observatories. M31N 2010-07b is located
at R.A. = 0h43m07s.50, Decl. = +41o17'58".6 (equinox 2000.0), which is
261" east and 110" north of the center of M31. Available R-band magnitudes
for M31N 2010-07b, measured by Hornoch: 2005 June 11.211 UT, [22.0 (D.
Mackey, 2.54-m Isaac Newton Telescope + narrow-band H_alpha filter); Oct.
8.369, [22.9 (P. Garnavich and C. Kennedy, 1.83-m Vatican Advanced Technology
Telescope + R filter); 2010 Jan. 31.784, [21.9 (P. Kubanek, N. Morales, J. L.
Ortiz, J. Gorosabel, and M. Jelinek, 1.23-m telescope at Calar Alto + R
filter); June 4.135, R = 20.7 +/- 0.2 (Morales, Ortiz, Gorosabel, Kubanek,
and Jelinek, 1.23-m telescope at Calar Alto); 9.459, R = 20.9 +/- 0.3
(Garnavich, C. Littlefield, N. Paul, and S. Bouzid, 1.83-m Vatican Advanced
Technology Telescope); 17.152, R = 20.8 +/- 0.2 (Kubanek, Gorosabel, O. Lara
Gil, and Jelinek, 1.23-m telescope at Calar Alto); July 10.200, Sloan r' =
20.9 +/- 0.2 (Corral-Santana and Casares, 2.54-m Isaac Newton Telescope);
10.210, [H_alpha] = 18.8 +/- 0.15 (Corral-Santana and Casares); 11.210,
Sloan r' = 20.9 +/- 0.2 (Corral-Santana and Casares); 19.186, Sloan r' =
20.8 +/- 0.2 (D. Pinfield, B. Sipocz, and G. Kovacs, 2.54-m Isaac Newton
Telescope); 19.191, [H_alpha] = 18.7 +/- 0.15 (Pinfield, Sipocz, and Kovacs);
20.069, [H_alpha] = 18.8 +/- 0.15 (Gorosabel, Lara Gil, Jelinek, Kubanek, and
P. Martorell, 1.23-m telescope at Calar Alto). When comparing measurements
in Sloan r' and H_alpha, they notice strong excess in H_alpha emission,
suggesting that the object is a nova well after the outburst.

Hornoch also reports additional R-band photometry of recent M31 novae as
measured by himself from images taken with the 0.65-m telescope at Ondrejov.
Magnitudes for M31N 2010-05a (cf. CBETs 2305, 2319, 2341, and 2391): July
9.035 UT, 18.6 +/- 0.15 (Hornoch and M. Wolf); 26.985, 19.2 +/- 0.2 (Hornoch);
28.051, 19.2 +/- 0.2 (Hornoch and Wolf).
R-band magnitudes for M31N 2010-06a (cf. CBETs 2341 and 2391): July
19.041 UT, 18.0 +/- 0.1 (Hornoch and P. Kusnirak); 20.070, 18.0 +/- 0.1
(Hornoch); 21.066, 18.0 +/- 0.1 (Kusnirak); 22.012, 17.8 +/- 0.1 (Hornoch and
P. Zasche); 26.950, 18.5 +/- 0.1 (Hornoch); 28.015, 18.3 +/- 0.1 (Hornoch and
Wolf); 28.051, 18.2 +/- 0.15 (Hornoch and Wolf); 29.044, 18.1 +/- 0.1
(Hornoch, Hornochova, and Zasche); Aug. 1.089, 18.5 +/- 0.1 (Kusnirak).
R-band magnitudes for M31N 2010-06b (cf. CBETs 2342 and 2391): July
19.041 UT, 19.0 +/- 0.15 (Hornoch and Kusnirak); 20.070, 18.7 +/- 0.1
(Hornoch); 21.066, 18.6 +/- 0.1 (Kusnirak); 22.012, 18.7 +/- 0.1 (Hornoch and
Zasche); 26.950, 19.4 +/- 0.15 (Hornoch); 28.015, 19.4 +/- 0.15 (Hornoch and
Wolf); 29.044, 19.6 +/- 0.15 (Hornoch, Hornochova, and Zasche); Aug. 1.089,
19.8 +/- 0.2 (Kusnirak).
R-band magnitudes for M31N 2010-06c (cf. CBETs 2343 and 2391): July
9.011 UT, 18.5 +/- 0.1 (Hornoch and Wolf); 14.050, 18.9 +/- 0.15 (Hornoch,
Wolf, and P. Hornochova); 15.010, 18.9 +/- 0.1 (Hornoch and Wolf); 17.062,
19.1 +/- 0.15 (Hornoch and Hornochova); 19.041, 19.3 +/- 0.15 (Hornoch and
Kusnirak); 20.070, 19.3 +/- 0.1 (Hornoch); 21.066, 19.2 +/- 0.15 (Kusnirak);
22.012, 19.3 +/- 0.15 (Hornoch and Zasche); 26.950, 19.6 +/- 0.2 (Hornoch);
28.015, 20.0 +/- 0.2 (Hornoch and Wolf); 29.044, 19.9 +/- 0.1 (Hornoch,
Hornochova, and Zasche); Aug. 1.089, 20.2 +/- 0.2 (Kusnirak).
R-band magnitudes for M31N 2010-06d (cf. CBETs 2347 and 2391): July
9.011 UT, 19.4 +/- 0.15 (Hornoch and Wolf); 9.035, 19.3 +/- 0.15 (Hornoch
and Wolf); 14.050, 19.3 +/- 0.25 (Hornoch, Wolf, and Hornochova); 15.010,
19.2 +/- 0.15 (Hornoch and Wolf); 17.062, 19.6 +/- 0.2 (Hornoch and
Hornochova); 19.041, 19.7 +/- 0.25 (Hornoch and Kusnirak); 20.070, 18.2
+/- 0.1 (Hornoch); 21.066, 17.7 +/- 0.1 (Kusnirak); 22.012, 17.7 +/- 0.1
(Hornoch and Zasche); 26.950, 19.0 +/- 0.15 (Hornoch); 28.015, 19.5 +/- 0.2
(Hornoch and Wolf); 28.051, 19.5 +/- 0.15 (Hornoch and Wolf); 29.044, 19.5
+/- 0.15 (Hornoch, Hornochova, and Zasche); Aug. 1.089, 19.5 +/- 0.15
(Kusnirak).
R-band magnitudes for M31N 2010-07a (cf. CBETs 2358 and 2391): July
19.041 UT, 17.2 +/- 0.1 (Hornoch and Kusnirak); 20.070, 17.11 +/- 0.05
(Hornoch); 21.066, 17.1 +/- 0.1 (Kusnirak); 22.012, 17.1 +/- 0.1 (Hornoch
and Zasche); 26.950, 16.9 +/- 0.1 (Hornoch); 28.015, 16.69 +/- 0.07
(Hornoch and Wolf); 28.051, 16.62 +/- 0.08 (Hornoch and Wolf); 29.044,
16.13 +/- 0.06 (Hornoch, Hornochova, and Zasche); Aug. 1.089, 16.53 +/-
0.10 (Kusnirak).

NOTE: These 'Central Bureau Electronic Telegrams' are sometimes
superseded by text appearing later in the printed IAU Circulars.

2010 August 13 (CBET 2411) Daniel W. E. Green

[Tikhon]

14 August 2010
IAU Electronic Telegram No.2412

POSSIBLE NOVA IN M31: M31N 2010-08a

Rafael Ferrando, Segorbe, Spain, reports his discovery of an apparent
nova (mag about 18.5) in M31 from five 120-s unfiltered CCD frames (limiting
mag 20.0) taken around Aug. 8.16 UT with a 0.40-m f/10 Ritchey-Chretien
reflector, the new object located at R.A. = 0h43m28s.28, Decl. = +41d41'25".0
(equinox 2000.0 assumed, not stated). A possible faint object is visible at
this location on an image from 2009 Aug. 26.13, which is posted by Ferrando
at the following website URL: http://pladearguines.com/NOVAM31-20100808.gif.
Additional unfiltered CCD magnitudes by Ferrando for M31N 2010-08a: Aug.
10.005, 18.2; 14.153, 17.9. Other Spanish observers have reported unfiltered
CCD magnitudes for M31N 2010-08a: Aug. 8.109, 18.5 (Carlos Segarra, Algimia,
0.20-m f/4 reflector); 8.137, 18.5 (Felipe Pena, Atzeneta del Maestrat,
0.15-m f/5 reflector); 10.057, 18.3 (Segarra; position end figures 28s.30,
25".2); 11.137, 18.1 (Angel de la Hermosa, El Boalo, Madrid, 0.35-m f/10
Schmidt-Cassegrain reflector; position end figures 28s.28, 24".9; image
posted at URL http://img228.imageshack.us/img228/4929 ... 010811.jpg).

NOTE: These 'Central Bureau Electronic Telegrams' are sometimes
superseded by text appearing later in the printed IAU Circulars.

2010 August 14 (CBET 2412) Daniel W. E. Green

[Tikhon]

16 August 2010
IAU Electronic Telegram No.2413

SUPERNOVA 2010gx

A. Pastorello, S. J. Smartt, M. T. Botticella, L. Magill, D. Young,
S. Valenti, and R. Kotak, Queen's University, Belfast, on behalf of the PS1
Collaboration (see, e.g., CBETs 1617, 1988, 2214), report that a luminous
optical transient detected by three wide-field surveys has evolved into a
type-Ic supernova. The Catalina Real Time Transient Survey first announced
the discovery of an optical transient (designated as CSS 100313:112547-084941)
at R.A. = 11h25m46s.71, Decl. = -8d49'41".4 (equinox 2000.0; cf. Mahabal
and Drake 2010, website URL http://www.astronomerstelegram.org/?read=2490 and
/?read=2508), on Mar. 13 (at SDSS r magnitude 18.6), and subsequently the
"Palomar Transient Factory" (PTF) collaboration reported an independent
discovery on images obtained during Mar. 5-16 (and designated PTF10cwr;
Quimby et al. 2010, URL http://www.astronomerstelegram.org/?read=2492).
Pastorello et al. (2010, http://www.astronomerstelegram.org/?read=2504) noted
that the transient was also detected by PS1 in the course of the 3Pi survey
during Mar. 12-23 (which they designated PS1-1000037). Early spectra by the
CRTS, PTF, and PS1 teams all indicated a blue continuum with broad O II
features and a host-galaxy (SDSS J112546.72-084942.0) redshift of z = 0.23.
The host redshift implies a very luminous transient (absolute mag < -21),
and the spectra were similar to the "ultra-bright" supernova 2005ap (see
http://www.astronomerstelegram.org/?read=2490, /?read=2508, /?read=2492,
/?read=2504; also, Quimby et al. 2007, Ap.J. 668, L99). Further detailed
spectroscopic monitoring with the Gemini South telescope and the William
Herschel Telescope by the PS1 team shows that -- 25 days after discovery --
the transient (here designated supernova 2010gx) evolved unambiguously into
a type-Ic event with the characteristic broad Fe II, Si II, Mg II, and Ca II
features. The spectra at +25 days are most similar to those of SN 1994I
(at six days before peak; Baron et al. 1996, MNRAS 279, 799) and SN 2003jd
(at peak; Valenti et al. 2008, MNRAS 383, 1485). This indicates a link
between the "ultra-bright" optical transients and type-Ic supernovae;
further details are reported by Pastorello et al. (2010, Ap.J., submitted).

NOTE: These 'Central Bureau Electronic Telegrams' are sometimes
superseded by text appearing later in the printed IAU Circulars.

2010 August 16 (CBET 2413) Daniel W. E. Green

[Tikhon]

17 August 2010
IAU Electronic Telegram No.2414

SUPERNOVA 2010gy

R. Chornock, Harvard-Smithsonian Center for Astrophysics (CfA); M. Huber,
Johns Hopkins University (JHU); R. J. Foley, M. Brodwin, and J. Ruel, CfA;
A. Rest, Space Telescope Science Institute; G. Narayan, E. Berger, P. Challis,
R. P. Kirshner, A. M. Soderberg, and C. Stubbs, CfA; M. Fraser and S. J. Smartt
Queen's University, Belfast; Y. Urata, National Central University, Jung-Li;
J. Tonry, Institute for Astronomy (IfA); A. Riess, JHU; W. M. Wood-Vasey,
University of Pittsburgh; P. A. Price, Princeton University; and E. Magnier, K.
Chambers, N. Kaiser, J. Morgan, W. Burgett, J. Heasley, W. Sweeney, C. Waters,
and H. Flewelling, IfA, report the discovery of a low-redshift type-Ia
supernova in the Pan-STARRS1 Medium Deep Survey. The object (designated
PS1-1000385 with the survey) was discovered at g = 20.8 (AB magnitude) on Aug.
5.59 UT at R.A. = 2h27m12s.036, Decl. = -4d32'04".87 (equinox 2000.0). The
previous non-detection had a 3-sigma upper limit of magnitude z = 23.0 on July
30.6. The transient has subsequently risen in brightness to magnitude g =
18.4 on Aug. 14.6. No clear host galaxy is associated with this transient.
The nearest object present in either the PS1 images or archival Canada-France-
Hawaii Telescope imaging is the source VVDS 20208952 (magnitude g = 24.5; see
http://vizier.cfa.harvard.edu/viz-bin/V ... ce=II/286/
vcat&VVDS=20208952).
A spectrum (range 340-860 nm) was obtained on Aug 14.4 using IMACS on
the Magellan Baade 6.5-m telescope, which revealed the transient to be a
normal type-Ia supernova near maximum light. Cross-correlation with a library
of supernova template spectra using the SNID program (Blondin and Tonry 2007,
ApJ, 666, 1024) finds a best-fit redshift of z = 0.06 and an age of 2 (+/- 3)
days before maximum light. The true host galaxy remains uncertain and is
either a very low-luminosity dwarf galaxy or is located far from the supernova.
The PS1 and Magellan telescope staffs are thanked for their assistance
with these observations. This discovery was enabled using the PS1 System,
operated by the PS1 Science Consortium (PS1SC) and its member institutions,
and made possible through the PS1 Builders (see the following website URL
http://www.ps1sc.org/PS1_System_IAU.shtml).

NOTE: These 'Central Bureau Electronic Telegrams' are sometimes
superseded by text appearing later in the printed IAU Circulars.

2010 August 17 (CBET 2414) Daniel W. E. Green

[Tikhon]

17 August 2010
IAU Electronic Telegram No.2415

SUPERNOVA 2010gz IN NGC 599

S. Nakano, Sumoto, Japan, reports the discovery by Masaki Tsuboi
(Kuchita-minami, Asakita-ku, Hiroshima) of an apparent supernova (mag 16.0)
on a 30-s unfiltered CCD frame taken on Aug. 16.782 UT using a 0.30-m f/5.3
reflector; Tsuboi obtained confirming images (limiting mag 19.0) on Aug.
16.78 and 17.61 UT and measures the new object to be located at R.A. =
1h32m51s.07, Decl. = -12d11'21".5 (equinox 2000.0), which is 39".6 west and
6".7 north of the center of NGC 599. Nothing is visible at this position on
Digitized Sky Survey red, blue, and infrared images (limiting mag 19 or
fainter). The discovery image has been posted at the following website URL:
http://ytenku.hp.infoseek.co.jp/astroph ... 817-01.jpg. Nakano
measured mag 15.2 and position end figures 51s.05 +/- 0s.01, 21".7 +/- 0".2
for 2010gz from Tsuboi's FITS images

NOTE: These 'Central Bureau Electronic Telegrams' are sometimes
superseded by text appearing later in the printed IAU Circulars.

2010 August 17 (CBET 2415) Daniel W. E. Green

[Tikhon]

17 August 2010
IAU Electronic Telegram No.2416

2010 PERSEID METEORS

P. Jenniskens, SETI Institute, reports that Geert Barentsen (Armagh
Observatory) has pointed out that the International Meteor Organization's
summary of visual meteor observations (which can be viewed at website URL
http://www.imo.net/live/perseids2010/#peak) shows that the Perseid rate
increased around Aug. 12d17h18m +/- 32m UT by about 60 +/- 15 meteors/hr (ZHR)
above normal annual shower activity levels on that date (solar longitude
139.748 +/- 0.022 deg, equinox 2000.0), in good agreement with predictions for
the earth's crossing of the 1479 dust ejecta from comet 109P/Swift-Tuttle
(cf. CBET 2401). The predicted peak rate was ZHR = 65 meteors/hr (Jenniskens,
2006, *Meteor Showers and their Parent Comets*, p. 657). These data are
based on roughly ten visual observers located in China, Russia, Japan, and
Israel.
S. Nakano, Sumoto, Japan, forwards the following visual counts by
Katsuhiko Mameta (Kobe, Hyogo-ken) at Nishi-Harima Observatory on Aug. 12
(limiting mag 6.0-6.3): 15h30m-16h00m UT, 22 Perseids, 10 other meteors;
16h00m-16h50m, 29 Perseids, 17 others; 18h05m-19h00m, 37 Perseids, 17 others.

NOTE: These 'Central Bureau Electronic Telegrams' are sometimes
superseded by text appearing later in the printed IAU Circulars.

2010 August 17 (CBET 2416) Daniel W. E. Green