New Comet: C/2013 P4 (PANSTARRS)

Cbet nr. 3638, issued on 2013, August 26, announces the discovery of a new comet (discovery magnitude ~20.8) by professional survey F51 Pan-STARRS 1 (Haleakala) on CCD images obtained with 1.8-m Ritchey-Chretien on August 15, 2013. After posting on the Minor Planet Center's NEOCP webpage, other CCD astrometrists have commented on the object's cometary appearance. The new comet has been designated C/2013 P4 (PANSTARRS).

We performed follow-up measurements of this object, while it was still on the neocp. Stacking of 9 R-filtered exposures, 60-sec each, obtained remotely, from the Faulkes Telescope South (Siding Spring) on 2013, August 26.5, through a 2.0-m f/10.0 Ritchey-Chretien + CCD (operated by Las Cumbres Observatory Global Telescope Network), shows that this object is a comet: sharp central condensation surrounded by a coma about 15" in diameter elongated in PA 190.

Below our confirmation image. Click on it for a bigger version.

M.P.E.C. 2013-Q34 assigns the following preliminary parabolic orbital elements to comet C/2013 P4: T 2015 June 23.59; e= 1.0; Peri. = 157.50; q = 4.40;  Incl.= 4.33

by Ernesto Guido, Kris Rochowicz, Nick Howes

Possible Bright Nova in Delphinus

Following the posting on the Central Bureau's Transient Object Confirmation Page about a possible Bright Nova in Del (TOCP Designation: PNV J20233073+2046041) we performed some follow-up of this object through a 0.43-m f/6.8 astrograph + CCD from MPC Code I89 (iTelescope network - Nerpio, Spain) and through a 0.25-m f/6.3 Schmidt-Cassegrain + CCD from MPC code C82 (Sorrento, Italy).

On our images taken on August 14.8, 2013 from MPC I89 we can confirm the presence of an optical counterpart with unfiltered CCD magnitude 6.8 at coordinates:

R.A. = 20 23 30.72, Decl.= +20 46 03.4

(equinox 2000.0; UCAC-3 catalogue reference stars).

On our images taken on August 14.8, 2013 from MPC C82 we can confirm the presence of an optical counterpart with unfiltered CCD magnitude 6.9 and R-Filtered magnitude 6.1 at coordinates:

R.A. = 20 23 30.68, Decl.= +20 46 03.7

(equinox 2000.0; CMC-14 catalogue reference stars).

Our confirmation image (click on it for a bigger version): 

An animation showing a comparison between our confirmation image and the archive POSS2/UKSTU plate (R Filter - 1990). Click on the thumbnail for a bigger version:

UPDATE - August 15, 2013

  

According to Cbet No. 3628, PNV J20233073+2046041 is now NOVA DELPHINI 2013. This nova has been discovered by Koichi Itagaki (Teppo-cho, Yamagata, Japan) on an unfiltered CCD frame taken on Aug. 14.584 UT using a 0.18-m reflector.

According to ATel #5279 an optical spectrum of NOVA DELPHINI 2013 was obtained (through patchy cloud) by the FRODOSpec instrument on the 2m robotic Liverpool Telescope on La Palma at 2013 August 14.909. The spectrum contains strong Balmer series emission exhibiting P Cygni profiles with velocities ~2000 km/s. A number of Fe II (also P Cygni profiles) and (weak) He I lines may be present. This object is likely to be a newly erupting classical nova (in the early fireball stage). A grating spectra, obtained by S. N. Shore et Al. on 2013 Aug. 14.87 with the coude spectrograph at the 2 meter Zeiss telescope of the Ondrejov Observatory, shows strong H-alpha emission with a P Cyg profile extending to a maximum radial velocities of -2300 km/s (absorption, EW approx 8.1A) and +2400 km/s (emission, EW \approx 52.9A) with no terminal edge at high negative velocity. The spectrum is typical of a classical nova -- possibly CO type -- in the early (optically thick) fireball stage but with indications of the onset of the recombination event.

UPDATE - August 17, 2013

According to the preliminary light-curve from AAVSO (see image below), NOVA DELPHINI 2013 reached a peak V magnitude ~ 4.3 on August 16.4.

Credit: AAVSO

Some interesting remarks about the nova are included in the ATel #5297 by Munari et Al.:

"Nova Del 2013 seems to have reached maximum brightness on August 16.45 UT at V=4.3 mag. It immediately entered the decline phase and it is declining pretty fast, of the order of 1 mag in a day, qualifying it as a very fast nova if the pace will be maintained on the coming days. Also the rise toward maximum has been real fast, 2 mag in about 1.5 days according to our photometry and AAVSO database. The total outburst amplitude is 12.6 mag in V, adopting V=16.9 mag for the progenitor as given by GSC 2.3.2."

Our image and animation showing the difference in brightness of NOVA DELPHINI 2013 between August 14.83 (V mag. ~6.3)  and August 15.93 (V mag. ~5.1). Images obtained with the same instrumentation and exposures. Click on the image for a bigger version.

Click on the thumbnail for a bigger version of the animation.

Below you can see a spectrum of NOVA DELPHINI 2013 obtained by M. Fulle on August 16 with a f=180mm f/2.8 with Star Analyser 100, 10x10-second exposure at 6400ISO (click on it for a bigger version).

Credit: M. Fulle

While below there is a normalized spectra obtained by Fujii-san on August 15, 2013 (click on it for a bigger version).

Credit: Fujii-san

UPDATE - August 18, 2013

According to Taichi Kato on [vsnet-alert 16230], NOVA DELPHINI 2013 reached a plateau, no fading.

The most recent AAVSO data indicate that the nova stopped fading (or even slightly brightened), and currently stays slightly above mag 5.0.  This behavior is consistent with Fujii-san's spectrum, which showed features of a premaximum nova. This nova is not a very fast nova as reported in ATEL 5297 (Munari et al.).

by Ernesto Guido, Nello Ruocco and Nick Howes

New Comet: C/2013 P2 (PANSTARRS)

Cbet nr. 3621, issued on 2013, August 07, announces the discovery of an apparently asteroidal object (discovery magnitude ~19.5) by professional survey F51 Pan-STARRS 1 (Haleakala) on CCD images obtained with 1.8-m Ritchey-Chretien on August 04, 2013 (pre-discovery Pan-STARRS1 observations from July 26 were found later by P. Veres). 

After posting on the Minor Planet Center's NEOCP webpage, this apparently asteroidal object as been found to show cometary features by astrometric observers elsewhere (including our team). The new comet has been designated C/2013 P2 (PANSTARRS).

We performed follow-up measurements of this object, while it was still on the neocp. Stacking of 30 R-filtered exposures, 40-sec each, obtained remotely from iTelescope network (MPC code H06, New Mexico) on 2013, August 06.3, through a 0.43-m f/6.8 astrograph + CCD + f/4.5 focal reducer, shows that this object is a comet: coma about 5" in diameter elongated in PA 120.

Below you can see our image. Click on it for a bigger version.

M.P.E.C. 2013-P42 assigns the following preliminary parabolic orbital elements to comet C/2013 P2: T 2014 Feb. 17.50; e= 1.0;  Peri. = 105.19; q = 2.83;  Incl.= 125.54

by Ernesto Guido & Nick Howes

Close Approach of Asteroid 2013 PJ10

M.P.E.C. 2013-P39, issued on 2013 August 06, reports the discovery of the asteroid 2013 PJ10 (discovery magnitude 14.8) by La Sagra Sky Survey (MPC code J75) on images taken on August 04.9 with a 0.45-m f/2.8 reflector + CCD.

2013 PJ10 has an estimated size of 31 m - 70 m (based on the object's absolute magnitude H=24.6) and it had a close approach with Earth at about 1 LD (Lunar Distances = ~384,000 kilometers) or 0.0025 AU (1 AU = ~150 million kilometers) at 0218 UT on 2013, August 04. This asteroid reached the peak magnitude ~13.0 on August 04.

We performed some follow-up measurements of this object on 2013, August 06.3, while it was still on the neocp, remotely from the H06 iTelescope network (New Mexico, Mayhill), through a 0.25-m f/3.4 reflector + CCD. Below you can see our image, stack of 6X15-second exposures, taken with the asteroid at magnitude ~15.3 and moving at ~ 19.0 "/min. At the moment of the close approach 2013 PJ10 was moving at ~ 218"/min. Click on the image below to see a bigger version. North is up, East is to the left

by Ernesto Guido & Nick Howes

Close Approach of Asteroid 2003 DZ15

M.P.E.C. 2013-O29, issued on 2013 July 20, reports the recovery of the Apollo asteroid 2003 DZ15 (magnitude 18) by F51 Pan-STARRS 1, Haleakala, on images taken on July 19.4 with a 1.8-m Ritchey-Chretien + CCD.

2003 DZ15 was discovered on February 2003 by 608 Haleakala-NEAT/MSSS and it has an estimated size of 95 m - 210 m (based on the object's absolute magnitude H=22.2) and it will have a close approach with Earth at about 9.1 LD (Lunar Distances = ~384,000 kilometers) or 0.0233 AU (1 AU = ~150 million kilometers) at 0037 UT on 2013 July 30. This asteroid will reach the peak magnitude ~16.5 on 29 and 30 July 2013. This is its closest approach to the Earth for this century, although it will make a pass nearly as close to the Earth in 2057 on February 12th.

We performed some follow-up measurements of this object, from the Q62 ITelescope network (Siding Spring, AU) on  2013, July 28.6, through a 0.50-m f/6.8 astrograph + CCD + focal reducer. Below you can see our image, single 120-second exposure, taken with the asteroid at magnitude ~16.6 and moving at ~40.80 "/min. At the moment of the close approach 2003 DZ15 will move at ~52 "/min. Click on the image below to see a bigger version (the asteroid is trailed in the image due to its fast speed).

Below you can see a short animation showing the movement of 2003 DZ15 (three consecutive 120-second exposure). Click on the thumbnail for a bigger version:

by Ernesto Guido & Nick Howes

SUPERNOVA 2013ej IN M74

Following the posting on the Central Bureau's Transient Object Confirmation Page about a possible Supernova in M74 (TOCP Designation: PSN J01364816+1545310) we performed some follow-up of this object remotely through a 0.43-m f/6.8 astrograph + CCD of iTelescope network (MPC Code  Q62 - Siding Spring, AU).

On our images taken on July 27.7, 2013 we can confirm the presence of an optical counterpart with R-filtered CCD magnitude 13.0 and V-filtered CCD magnitude 12.6 at coordinates:

R.A. = 01 36 48.20, Decl.= +15 45 31.0

(equinox 2000.0; UCAC-3 catalogue reference stars).

Our annotated confirmation image (single 120-second exposures under a cloudy sky):

An animation showing a comparison between our confirmation image and the archive POSS2/UKSTU plate (R Filter - 1990). Click on the thumbnail for a bigger version:

UPDATE - July 28, 2013

According to CBET 3606 this transient has been discovered by LOSS supernova survey on unfiltered KAIT images obtained on July 25.45.

D. D. Balam, Dominion Astrophysical Observatory, National Research Council of Canada; M. L. Graham, Las Cumbres Observatory Global Telescope, University of California at Santa Barbara; and E. Y. Hsiao, Las Campanas Observatory, report that a spectrogram (range 369-700 nm, resolution 0.3 nm) of PSN J01364816+1545310 = SN 2013ej, obtained on July 27.41 UT with the 1.82-m Plaskett Telescope of the National Research Council of Canada, shows a moderately blue continuum with weak Balmer emission lines showing P-Cyg profiles, suggesting that this is a core-collapse event.

This young type II supernova has been officially designated 2013ej.

This is the third supernova in M74 over the last eleven years (previous SN were: SN 2002ap and SN 2003gd).

Other info about this bright supernova are available through Atel (The Astronomer's Telegram):

ATel 5228: Spectroscopic classification for PSN J01364816+1545310 in M74 with FLOYDS at Faulkes Telescope South http://bit.ly/14loD8R  

ATel 5229: The Probable Progenitor of PSN J01364816+1545310 in M74 http://bit.ly/1bvU8XF

ATel 5230: Possible Spitzer Counterpart of PSN J01364816+1545310 http://bit.ly/12tjukY

Below you can see our image of supernova 2013ej IN M74 obtained on 2013 July 28.7. Click on it for a bigger version. (R-magnitude 12.8; B-magnitude 12.0)

by Ernesto Guido & Nick Howes

Observations of the Herschel Space Observatory

The Herschel Space Observatory was a European Space Agency-built and -operated space observatory, active from 2009 to 2013. It was studying the Universe by the light of the far-infrared and submillimeter portions of the spectrum revealing new information about the earliest, most distant stars and galaxies, as well as those closer to home in space and time. It has also taken a unique look at our own solar system. Herschel Space Observatory was the largest infrared telescope ever launched, carrying a single 3.5-metre mirror.

In the afternoon of April 29, 2013 Herschel ran out of liquid helium. To declare end-of-helium (EoHe) a number of key temperature sensor upper limits had been defined, and with two of them attained, EoHe had formally been reached. Herschel has made over 35000 scientific observations, amassing more than 25000 hours of science data from about 600 observing programmes. Finally on June 17, 2013, engineers for the Herschel space telescope sent final commands to put the decommissioned observatory from its orbit around the L2 point 1.5 million kilometres from the Earth into its “graveyard” heliocentric parking orbit.

Last week we decide to follow-up the "Herschel Space Observatory" in his new orbit using the Faulkes Telescopes (2.0-m f/10.0 Ritchey-Chretien + CCD - operated by Las Cumbres Observatory Global Telescope Network).  In fact, determining an accurate orbit now is important, because its increasing distance will make it fainter and much harder to keep track of in the intervening years.

"The observation was a particular challenge as the final manoeuvres made by the ESA flight control team resulted in the observatory being at a slightly different position on the sky compared to that predicted by existing orbital data".

We successfully imaged the Herschel on 26 & 27 June 2013 with Faulkes Telescope North and again on 01 July 2013 with the Faulkes Telescope South at magnitude ~20. (follow-up observations have been obtained by T. Vorobjov on June 28, 2013 at Kitt Peak - MPC code 695).  It was already a couple of arcminutes off prediction. See our image below, stacking of 7x120 seconds exposures (click on it for a bigger version).

Below you can see a short animation showing the movement of the Herschel Space Observatory during our first observing session of June 26, 2013. Click on the thumbnail for a bigger version.

Using our data, Bill Gray calculated for Herschel a return to opposition on 2027 Oct 24 +/- 4 at about 0.055 AU, reaching mag 22.  Below you can see the new orbit (click on the image for a bigger version).

Credit: Bill Gray

by Ernesto Guido & Nick Howes