Supernova 2002ap in M74

This page is devoted to information on Supernova 2002ap in M74 Basic information on this SN, including the last reported brightness, on this Supernova can be found on the main page.  Information on the original web pages for many of these images can be found on the updates and links web pages.

Discovered by Japanese amateur Yoji Hirose during a full moon. (just like 1998bu). The spectrum of this thing looks interesting. It has similarities to 1998bw which was a GRB canditate.  This is a rare type of Ib/c supernovae called a Hypernova.  Maximum brightness 12.3 was reached on February 12th. The expected maximum was around mag 10. We have a DSS Photometry reference image made by Odd Trondal. Icon generated from the CfA image.

Web pages dedicated to this SN.
• VSNET has a 2002ap page (2002ap summary page)
• SEDS has a 2002ap page.
• AAVSO has posted News Flash #904, and Special Edition, 2002ap.
  • finder charts
• Reinder Bouma finder chart
• AUDE has a 2002ap page in French [Translate]
• M1 SN search has a 2002ap page.
• CometMan's 2002ap page.
• H. Motegi 2002ap page in Japanese [Translate]
• Bruce L. Gary's 2002ap page

The following is a list of images of this SN, in chronological order. Click on the name in the "observer" column to see the image. Times and dates are in UT unless otherwise noted. If you know of any others, please tell me! RGBC

Image Credit	Date	Mag	Filter	Comments
INT image	2001/07		C	Progenitor, (in field?)
William Rogers image	2002/01/29.04	15.2	C	Pre Discovery
LOTOSS image	2002/01/29.2	14.4	C	Confirmation
Yasuo Sano image	2002/01/31.375	13.4	C	mirror, local mirror
Josch Hambsch image	2002/01/31.751	13.6	C
Diego RodrМguez image	2002/01/31.776	13.5	V
Seikei High school image	2002/02/01.425		C
CfA image	2002/02/01		BVI	color, WOW
Kamila Hornocha image	2002/02/01		R
Tom McMahon image	2002/02/01.597	13.2	C
Rezman Obs image	2002/02/01.737		C	local mirror
Rafael Ferrando image	2002/02/01.783	13.1	CR	local mirror
Scutum Obs image	2002/02/01.8		C	local mirror
Ljubljana High school image	2002/02/01.804	13.5	C
JM Llapasset image	2002/02/01.810	13.2	CR
Gyula P. Szokoly image	2002/02/01.819	12.45	K	FITS format, notes
Gyula P. Szokoly image	2002/02/01.825	12.61	J	FITS format, notes
Cedric Leyrat image	2002/02/01.917	13.2	CR
Larry Robinson image	2002/02/02.094		C
Rob Simcoe and Josh Bloom image	2002/02/02.107	13.1	V
Rob Simcoe and Josh Bloom image	2002/02/02.115	13.2	R
Esteban Reina Lorenz image	2002/02/02.184	13	C
Paul Gitto image	2002/02/02		C	Comparison image
Ondrej Pejcha and P. Sobotka image	2002/02/02		VRI	color
Rezman Obs image	2002/02/02		C
Wendelstein Obs image	2002/02/02		BVI	color
Paolo Corelli image	2002/02/02.745	12.4	G	RGB image
Josch Hambsch image	2002/02/02.750	12.7	C
Rafael Ferrando image	2002/02/02.780	12.95	CR	local mirror
J. Nicolas image	2002/02/02.807	13.0	CR
Josep M. Bosch image	2002/02/02.810	12.9	CR
P. Dubreuil image	2002/02/02.817	13.0	CR
Ole Nielsen image	2002/02/02.826	12.7	C
Gyula P. Szokoly image	2002/02/02.827	12.22	K	FITS format, notes
Gyula P. Szokoly image	2002/02/02.832	12.46	J	FITS format, notes
Joaquin and Yago Ferreiros	2002/02/02.858	13.0	V	V filter image
Remanzacco Obs	2002/02/02.900		C	local mirror, mirror
Paul Gitto image	2002/02/03.015	12.4	C	comparison image
Kopernik image	2002/02/03.042	13.36	C
Rolando Ligustri image	2002/02/03	12.5	C
Gianluca Masi image	2002/02/03.760	12.9	R
Piergiorgio Ferrante image	2002/02/03.761	12.7	C	local mirror
Scutum Obs image	2002/02/03.8		C	local mirror
Philip Keller and Christian Fuchs image	2002/02/04		RGB	color, wow!
P. Dubreuil image	2002/02/03.881	12.8	CR
Kereszty Zsolt image	2002/02/04		C	color version
Wise Obs image	2002/02/04?		RGB	Color
JM Llapasset image	2002/02/04.765	12.4	CR
Joel Nicolas image	2002/02/04.837	12.5	CR
Odd Trondal image	2002/02/04.888	12.4	CR
Fred Ewalt image	2002/02/05.016	12.3	C	color version
Stefan Lilge image	2002/02/05.743	12.1	C
Scutum Obs image	2002/02/05.8		C	local mirror
Matt Seegers image	2002/02/06		C
D Lefoulon image	2002/02/06.806	12.2	CR
Martin Mobberley image	2002/02/06.873		C	mirror
Paolo Corelli image	2002/02/07.761	12.1	C
J. Nicolas image	2002/02/07.785	12.3	CR
L. Brunetto image	2002/02/07.867	12.6	CR
John N. Gretchen III image	2002/02/08.125	12.6	C	color version
UMBC telescope image	2002/02/08		C	color
Arne Danielsen image	2002/02/08.770	12.5	CR
TorbjЬrn Fredriksen image	2002/02/08.759	12.68	C
JM Llapasset image	2002/02/08.774	12.2	CR
Rafael Ferrando image	2002/02/08.815	12.65	CR
Gerardo JimИnez image	2002/02/08.830	12.2	C
Pedro Re' image	2002/02/08.832	12.53	C	comparison images, Animated GIF
Pierre Dubreuil image	2002/02/08.833		C
Fred Ewalt image	2002/02/08.995	12.3	C	color version, comparison images
Richard Robinson image	2002/02/09.007	12.04	C
Phil Sullivan image	2002/02/09.350	12.31	V
Rafael Ferrando image	2002/02/09.780	12.60	CR
Nick James image	2002/02/09.786		C
KovАcs Attila image	2002/02/10		C
Tordai TamАs image	2002/02/10		C
Stig Foss image	2002/02/10.797	12.7	R
Kereszty Zsolt image	2002/02/10.788	12.34	V
JM Llapasset image	2002/02/11.764	12.2	CR
JM Llapasset image	2002/02/12.807	12.3	CR
J Nicolas image	2002/02/12.821	12.3	CR
J. Blanco image	2002/02/12.855		C
L. Brunetto image	2002/02/12.866	12.60	CR
Yasuo Sano image	2002/02/13.388	12.29	CR
Stig Foss image	2002/02/13.799	12.7	R
Pedro Re' image	2002/02/13.811	12.6	C
Martin Mobberley image	2002/02/13.865		C
Martin Mobberley image	2002/02/14.803		C	mirror
Fred Ewalt image	2002/02/15.023	12.46	C
Seikei High School image	2002/02/15.382	12.8	C
Martin Mobberley image	2002/02/15.809		C
Martin Mobberley image	2002/02/16.802		C
Martin Mobberley image	2002/02/18.786		C
J. Nicolas image	2002/02/18.807	12.6	CR
J. Nicolas image	2002/02/19.790	12.7	CR
Stig Foss image	2002/02/20.767	13.1	R
J. Nicolas image	2002/02/21.807	12.8	CR
JM Llapasset image	2002/02/22.770	12.8	CR
Rafael Ferrando image	2002/02/22.831	13.04	CR
John N. Gretchen III image	2002/02/23.041	12.957	C	color version
Rafael Ferrando image	2002/02/23.804	13.11	CR
J. Nicolas image	2002/02/24.812	13.0	CR
CROSS image	2002/02/25.80	13.36	C
Martin Mobberley image	2002/02/27.823		C
Rafael Ferrando image	2002/03/02.805	13.60	CR
JM Llapasset image	2002/03/03.775	13.5	CR
J Nicolas image	2002/03/03.790	13.4	CR
H. Motegi image	2002/03/04		C
JB. De Vanssay image	2002/03/04.824	13.4	CR
H. Motegi image	2002/03/07		C
Martin Mobberley image	2002/03/07.825		C
J Nicolas image	2002/03/07.819		CR
JM Llapasset image	2002/03/08.788		CR
R Poncy image	2002/03/10.793		CR
JM Llapasset image	2002/03/10.789	13.8	CR
J. Nicolas image	2002/03/10.797	13.8	CR
				Solar Conjunction
R Poncy image	2002/07/12.119	15.7	CR
F. Dubreuil image	2002/08/04.081		CR
JM Llapasset image	2002/08/13.117	16.6	CR
F. Dubreuil image	2002/08/14.012	16.5	CR	mirror
F. Dubreuil image	2002/08/14.026	16.61	CR
JM Llapasset image	2002/08/14.093	16.6	CR
JM Llapasset image	2002/08/14.106	16.3	Rc
Rezman Obs image	2002/08/18.094		C
J Nicolas image	2002/08/19.056	17.0	CR
F. Dubreuil image	2002/09/01.002	17.0	CR
A. Leroy image	2002/09/07.954	16.9	CR
Ota Observatory image	2002/09/11		CR
C. Dupuy image	2002/09/12.987	17.1	CR
A. Leroy image	2002/09/14.014	17.0	CR
JM Llapasset image	2002/09/16.063	17.0	CR
D. Lefoulon image	2002/09/17.109	17.2:	CR
A. Leroy image	2002/10/04.987	17.5	CR
C. Dupuy image	2002/10/05.004	17.5	CR
Josep M. Bosch image	2002/10/07.98		CR
Rafael Freeando image	2002/10/26.955	17.7	CR	Animated GIF showing asteroid 1998SY101
Fred Ewalt image	2002/10/29.090	18.2	CR
Derrick Farley image	2002/11/			color
Martin Mobberley image	2002/11/26.792	18.7	C	mirror, local mirror
Paulo Cacella image	2002/12/01.028			click here first
Fred Ewalt image	2002/12/21.991	19.25	C

Light curves and Spectra:
• Tautenburg 2-M telescope took this High resolution spectrum
• Dunlop Obs spectrum showing the progression of this supernova animated spectrum
• GAO Spectrum taken 2002/01/31.4 showing a precular type Ib/c
• Bisei Spectrum taken 2002/01/31.5
• La Palma Spectrum taken 2002/02/02
• Wise Observatory spectrum taken 2002/01/31
• Bruce L. Gary light curve
• "The Astronomer" has posted a Light curve
• MEDUZA has a light curve.
• Lew Cook light curve
• light curve in Postscript format, from Paul Vreeswijk (University of Amsterdam)
• Aude Measurements and light curve.
• VSNET Light curve (requires JAVA).

Other VSNet data on this SN (which will be copied here until VSNET gets it archive working again):
• [vsnet-campaign-sn 328] SN 2002ap in Messier 74 = NGC 628

  Dear SN watchers,

  A SN in M74 is discovered by Japanese amateur Yoji Hirose at mag 14.5 (on Jan 29.4) and rising (mag 13.7 on Jan. 30.38). Latest SN in Messier object is SN 1999gn in M61. If this new object is of type Ia, it can become mag 11, the brightest SN since SN 1993J in M81.

  Because I have no time for further noting, I give here the location only: R.A. = 1h36m23s.85, Decl. = +15o45'13".0 (2000.0, the KAIT result), which is about 258" west and 108" south of the face-on spiral (SA(s)c) galaxy M74 = NGC 628 in Pisces. The KAIT image can be seen at: http://astron.berkeley.edu/~bait/2002/sn2002ap.gif , and the chart can be found at AAVSO: http://www.aavso.org/charts/PSC/SN2002AP/ .

• [vsnet-campaign-sn2002ap 12] SN 2002ap in Messier 74 = NGC 628; further note

  Dear SN watchers,

  # As Kato-san noted, a subgroup "vsnet-campaign-sn2002ap" is created.
  # Please use this group for further discussion.  Only the noteworthy
  # reports will be appear on other subgroups (-alert, -campaign-sn).
  

  SN 2002ap seems brightening further. Y. Sano, Nayoro, Hokkaido, reports that it is mag 13.41 on Jan. 31.363 UT (unfiltered, compared with USNO-A2.0 rmag). It is surely rising.

  The new object locates on the outermost region of the spiral arm. There are many foreground stars superimposed on and around M 74. SN 2002ap locates between GSC 1205.789 and GSC 1205.744. Sano's image (ftp://ftp.kusastro.kyoto-u.ac.jp/pub/vsnet/SNe/sn2002ap/sano0131.jpg) will help the identification, as well as images in D. Bishop's page: http://www.RochesterAstronomy.org/sn2002/index.html#2002ap , and http://www.RochesterAstronomy.org/sn2002/sn2002ap.html .

  The comparison stars with V magnitude (measured by A. Henden) is available at AAVSO site http://www.aavso.org/charts/PSC/SN2002AP/ , or Tycho-2 Vmag based one is available at: http://www.shopplaza.nl/astro/vs-charts/sn2002ap.htm , which are very useful for a visual and V-filtered CCD observers. The unfiltered CCD observer, however, should use R magnitude or such. Temporary, USNO_A2.0 rmag would help.

                Henden-V USNOrmag note
  GSC 1205.1059   13.3    12.9    1' west of SN
  GSC 1205.789    13.9    13.5    2' west of SN
  

  The distance measure of M74 is about 29.5. The preliminary analysis of the spectrum (See vsnet-alert 7120) reveals very unusual feature, which resembles to that of "hypernova"! The follow-up observation in all wavelength is surely, strongly, highly recommended for this unique and very interesting exploding object!

• [vsnet-campaign-sn2002ap 9] finderchart SN 2002ap

  We have placed a finderchart (2.0 x 2.5 degrees field) of this bright SN with comparison stars down to magnitude 12.6 selected from Tycho-2, just in case it is type Ia, at the following URL: http://www.shopplaza.nl/astro/vs-charts/sn2002ap.htm

  A f-chart (15x15') with Arne Henden's 1-night photometry and comparison stars fainter than magnitude 12.1 is available at the AAVSO-site (http://www.aavso.org/charts/PSC/SN2002AP/).

  Reinder Bouma/Edwin van Dijk

• [vsnet-campaign-sn 332] SN 2002ap spectrum

  Dear SN watchers,

  I have submitted an article (below) to CBAT. SN 2002ap is a unique object!

  K. Kinugasa, H. Kawakita, Gunma Astronomical Observatory (GAO); K. Ayani, T. Kawabata, Bisei Astronomical Observatory (BAO); and H. Yamaoka, Kyushu University, write: "Low-resolution spectra of SN 2002ap (IAUC 7810) are obtained on Jan 31.4 UT with GAO 0.65-m telescope (with GCS, range 380-750 nm) and on Jan 31.5 UT with BAO 1.01-m telescope (range 470-700 nm). Preliminary reduction reveals rather blue continuum with a steep decreace over 650-700 nm, and without any deep absorption or emission. Very broad (FWZI ~ 30 - 50 nm) and shallow depressions exist around 570 nm (deepest), 470 nm, and 620 nm. Overall feature resembles to that of a peculiar Ib/c SN (or "hypernova") 1997ef, but SN 2002ap is much bluer. The follow-up observation in all wavelength is strongly recommended for this unusual and nearby exploding object. The spectra can be seen at: http://www.astron.pref.gunma.jp/images/gcs/SN2002ap.gif and http://www.town.bisei.okayama.jp/bao/astro/sn/sn2002ap.gif .

• [vsnet-campaign-sn2002ap 13] Re: SN 2002ap spectrum

  This information was announced on IAUC 7811, as well as other two spectrum (ESO and Wise Obs.), both of which reached the same conclution, i.e., SN 2002ap is a HYPERNOVA !

  The intensive followup observation of this unique and very nearby hypernova is strongly encouraged.

• [GCN GRB 1237] Type Ib/c SN2002ap (SN/GRB?) Radio Observations
• [GCN GRB 1238] Type Ib/c SN2002ap (SN/GRB?)
• [vsnet-campaign-sn2002ap 23] (fwd) Re: SN 2002ap spectrum (Deng)

  I am now modelling the Jan.31 spectrum sent to us by H. Yamaoka with a SN spectrum synthesis code, SYNOW. The observed broad features can only be explained when assuming very high expansion velocities for the ejecta material, like in SNe 1997ef and 1998bw. This in turn suggests very high explosion energy, higher than 1 times 10^52 ergs. So it is a hypernova.

  Jinsong Deng

• [vsnet-campaign-sn2002ap 33] Re: SN 2002ap spectrum

  >  I presume that the hypernova classification is based on its
  >luminosity (or total energy), rather than the spectrum.
  

  Another feature of hypernovae is a very (up to 30000 km/s or more) expansion velocity, derived both from the width and the blueshift of the absorption features (if identified).

  >  I wonder what would be the expected maximum magnitude (and when)
  >of this super/hypernova.
  

  It is not certain, but it would be as bright as, or somewhat brighter than, normal SN Ia. The maximum will be in next 20 days or so, but it is also uncertain. Keep your eyes on this exceptional object until it will go away.

• [vsnet-campaign-sn2002ap 35] [resend] Hypernova article

  I happened to write an article about hypernovae, for the publication of "2002 Special Bulletin of M 1 Group", on Jan. 24, 2002. What a coincidence! It is now in press and will be published this February, but by cortesy of the editor J. Ripero, I can introduce it here. It is very short article, so please have a fun.

  Next, I will write about the Galactic Supernova ;-).

  Sincerely Yours,
  Hitoshi Yamaoka, Kyushu Univ., Japan
  yamaoka@rc.kyushu-u.ac.jp
  

  ---
  Hypernovae: more energetic explosion than normal SNe

  H. Yamaoka (Kyushu University, Japan)

  The search for the supernovae (SNe) has always a possibility of the discovery of a object in the other category. It would be a comet (like C/1998 Y2 (Li) and C/1999 E1 (Li) by the Lick Observatory SN Search), or a Galactic cataclysmic variable (like KL Draconis, which was originally announced as SN 1998di). Hypernovae, however, are not in the other category but of the subclass of supernovae, which are the whole destruction of stars at their end of the life.

  The most impressive example of hypernovae is SN 1998bw. It was discovered by the ESO team, who were seeking the optical counterpart of the gamma-ray burst occured on Apr. 25, 1998. The spectrum of this object has some broad lines, which suggested that it is expanding with a high velocity, or, in the other word, exploding. The expansion velocity of this object reached 30000 km/s, i.e., 10 % of the speed of light.

  It does not resemble, however, to that of any known class of supernovae. The hydrogen lines are absent, thus it would be classified as type I. But no silicon line (typical for SN Ia) nor helium line (strong in SN Ib) are observed. Such supernovae are classified as SN Ic, but SN 1998bw did not resemble to the typical SNe Ic, such as SN 1994I in Messier 51. Then, this "supernova" is now classified as "peculiar type Ic". The expanding velocity and the light curve suggests that the explosion was occured sometime during Apr. 21-27, which supports the association of this SN with the gamma-ray burst.

  The other striking characteristics of SN 1998bw was its luminosity; it was more luminous than typical SNe Ia which are thought to be most luminous class among SNe. The energy source of SNe after explosion is a decay of the radioactive nuclei (mostly Nickel 56) produced during the explosion, so the amount of such matters would be larger in this object than the normal SNe. The light curve shows a slow evolution, which suggests that the large amount of material is ejected.

  On these basis, a "hypernova" model is constructed (Iwamoto et al., 1998, Nature). Very massive star (having 40 solar mass or more at birth) evolved losing its hydrogen-rich envelope and helium layer, then finally the gravitational core collapse occured. If the energy supplied by the collapse is 30 times larger than the typical core-collapse SNe, the amount of the produced radioactive nuclei are 10 times larger than a typical core collapser, or slightly larger than in a typical SN Ia. It also explains the higher expansion velocity. The central remnant would be a blackhole, which may ejected the "gamma-ray burst" during the collapse.

  Such hypernovae were searched from the previously discovered SNe. Then, from the resemblance of the spectrum and the light curve, it is now considered that SN 1997ef is also a hypernova though the coincident gamma-ray burst was not detected. This SN was discovered by Japanese amateur Yasuo Sano. You may be the next discoverer of hypernova! I hope your SN search and observation will reveal the new aspect of SN science.

• [vsnet-campaign-sn2002ap 43] SN 2002ap preliminary sequence (Henden)

  SN 2002ap preliminary sequence (Henden)

  The following message was relayed from Arne Henden, as originally posted to AAVSO-GRB:

  I've posted on ftp://ftp.nofs.navy.mil/pub/outgoing/aah/sequence/sn2002ap.dat a BVRI field photometry file from last night. Much as I begged the clouds to go away, there remained scattered cirrus at the time these observations were made. My estimate is perhaps a 0.1mag external error on these numbers.

  The photometry is inconsistent with the Vmag frame extraction that I gave Mike Simonsen to make the AAVSO chart for this field, with the new photometry about 0.25mag brighter at V. Brian Skiff was good enough to give me 3 stars that Harold Corwin measured many moons ago near the center of M74; that photometry was pretty poor, but indicated that the chart mags were too faint by 0.17mag. So bottom line is that I would trust the sn2002ap.dat magnitudes more than the current chart magnitudes, but both sets are under suspicion until a decent night is available.

  However, the supernovae does appear in the .dat file at

    RA  (J2000) DEC      RA             DEC       V     B-V    V-R    R-I
  24.099676  15.753692 01:36:23.92  +15:45:13.3 12.987  0.558  0.018 -0.212
  

  The spectra indicate a rather blue continuum with broad absorption at 448.0, 557.5, and 719.5 nm, or roughly the center of B and V, and inbetween R and I. Depending on the depths of these absorptions, the broadband colors can be almost anything, as evidenced above. VRI indicate a pretty blue object; B is fainter than expected, but probably due to the 448.0 absorption.

  Note that the position above is very close to the radio position, right-on in RA and 0.4arcsec off in DEC.

  Arne

• [vsnet-alert 7152] SN 2002ap
• [GCN GRB 1240] pre-SN2002ap (SN/GRB?) imaging of M74
• [GCN GRB 1242] SN 2002ap field phorometry
• [GCN GRB 1243] SN 2002ap spectrum
• [GCN GRB 1244] progenator image
• [GCN GRB 1247] SN2002ap (SN/GRB?) optical spectrographic observations
• [GCN GRB 1248] SN2002ap (SN/GRB?) Echelle spectra
• [GCN GRB 1312] SN 2002ap peak brightness date
• The Type Ic Hypernova SN 2002ap
• Wise Observatory paper on 2002ap