NOVA SAGITTARII 2014 Sigeru Furuyama, Japan reports discovery of a possible magnitude 8.7 nova in Sgr on two 10-s CCD frames (limiting magnitude 12.5) of 2014 Jan. 26.85UT using a 200-mm f/2.8 camera lens + BJ-42L camera. It is located at; RA 18h25m08s.60 DEC -22d 36' 02.4" (2000). Nothing was visible on numerous patrol frames of the same field taken since 2012 August.
Andrew Pearce, Nedlands, Western Australia, reports the following visual magnitude estimates Jan. 28.839, 10.5; Feb. 8.834, 10.9, 9.828, 10.8 (Pearce); 10.851, 9.8.
Akira Arai, Nishi-Harima Astronomical Observatory, University of Hyogo, reports that a low-dispersion spectrogram was obtained on Jan. 30.87 UT using the 2-m Nayuta telescope (+ MALLS). The spectrum shows emission lines at H-alpha (FWHM about 1200 km/s; EW about -70 nm), H-beta (EW about -13 nm), Na D, Fe II (multiplets 42, 48, 49, 55, 74), [O I] (557.7- 630.0-, and 636.4-nm), O I (777.3- and 844.6-nm), and the Ca II infrared triplet on a highly reddened continuum emission. Tiny absorption features are seen with the H-alpha and O I lines at about -1200 and -700 km/s, respectively. These results indicate that the object is a "Fe II"-type classical nova past maximum.
V809 CEPHEI Nick James reports it is just over a year since the discovery of the nova V809 Cep. He imaged it again on 2014 Feb 13 in V, Rc, Ic. The estimated mag is around Rc=18.2 using UCAC-4. The nova is also visible in the Ic frame but not V which has an LM of around 18.3. The nova is quite difficult to measure since it is only around 10 arcsec from a V=16.6 star.
SUPERNOVA 2014J IN M82: PROGENITOR S.C. Williams (Liverpool John Moores University) et. al. reports on The Astronomer's Telegram 5824 initial results of the search for a resolved progenitor of the recent Type Ia supernova in M82. Liverpool Telescope data taken using the IO:O CCD camera on 2014 January 26.91UT were used to constrain the position of the SN relative to a number of field stars. They conducted a search for the progenitor system using archival Hubble Space Telescope data (F435W, F555W and F814W) taken on 2006 March 27. In agreement with preliminary results in ATEL #5789, we find no resolved progenitor candidate coincident with the position of the supernova in any of the ACS/WFC data. We performed photometry on these data using DOPLHOT and hence derive the following limiting magnitudes F435W>23.3, F555W>23.4 and F814W>24.5 (based on photometry of nearby F435W>faint sources).
Recurrent Nova systems, such as RS Oph and T CrB, containing red giant secondaries, and U Sco, which harbours a sub-giant secondary, are a potential progenitor pathway to SN Ia. Assuming a distance to M82 of 3.5 +/-0.3 Mpc and either negligible reddening or E(B-V) = 1.2 (ATEL #5818), these upper photometric limits can be compared to a distance and extinction corrected SED</a> of known quiescent recurrent novae, including M31N 2008-12a with a one year inter-outburst time. Even assuming zero extinction, these limits do not rule out systems similar to any known Galactic or extragalactic recurrent (or fainter classical) novae from being the progenitor of SN 2014J.
SUPERNOVA 2014G IN NGC 3448 (KOICHI ITAGAKI) 2014G Jan 14.57 10 54 34.13 +54 17 56.9 15.6 44 "W 20 "S The discovery image was posted at URL: http://www.k-itagaki.jp/images/3448.jpg. Patrick Wiggins (Erda, USA) with a Celestron C14 reflector + SBIG ST-10XME camera) reports an independent discovery of this variable at mag about 17 from images apparently taken on Jan. 14.317 and 14.542 R. Itoh: spectrum Jan 14 good match to type-II supernovae close to maximum.
SUPERNOVA 2014H (TNTS) 2014H Jan 14.56 03 37 01.48 +32 05 01.7 16.8 0.2"E 9.2"N J.-J. Zhang: spectrum Jan 15 type-Ia a few days before maximum.
SUPERNOVA 2014I IN PGC 17633 (PARKER) 2014I Jan 17.52 05 42 19.80 -25 32 39.9 17.0r 15 "W 12 "S An image of the variable is visible via URL: http://tinyurl.com/kl4a876 M. Childress: spectrum Jan 18 type-Ia a few days before maximum
An ARAS web page is opened for this interesting campaign. One will find the targets, the objectives for each spectral resolution, and recommendation by Terryl Sergisson
#1 Information for those interested in beginningin Spectroscopy Section Sun Dec 09, 2012 4:34 pm by revandBellman • 4.874 Posts • messageSend message | profileView profile | onlinerevandBellman is online.| save quote --------------------------------------------------------------------------------
avatar A good place to start is to read about the different equipement available and how to use it, try Astronomical Spectroscopy for Amateurs by Ken Harrison, or his book on grating spectroscopes. After that it would be good to look at some website of people who are doing spectroscopy, such as http://www.threehill...pectroscopy.htm, http://www.astroman.fsnet.co.uk/spectro.htm For more info and software help and general assistance look at : http://astrosurf.com/buil (Christian Buil)
Dr. Martin indicates that the low resolution would be good to monitor the overall spectra and look for changes. High-resolution could then examine those line in detail. As I understand it, these stars are unpredictable and do many strange things that have not ben studied in detail. So periodic Star Analyser images, particularly of Betelgeuse would be great. Dr. Martine says emission lines periodically pop up, but it is hard to catch them. Comparing images should show changes. The trick will be to get a good technique so the spectrum images should be identical except for real spectral changes. This Project should be an excellent way to learn more about spectroscopy and to refine your techniques.
This campaign is on again this year, 2013/14. sorry its taken so long to get this up, but I lost the email when my account was hacked. The Orion Project web site is now up. Please see:http://www.hposoft.com/Orion/Orion.html
The Project is being coordinated with Dr. John Martin and Dr. Matt Templeton.
The Project focuses on 4 bright stars in Orion, Betelgeuse, Rigel, Mintaka and Alnilam. Other stars may be added in the future. Photometry and spectroscopy of one or more of these stars is requested. Because the stars are bright, they are easy for spectroscopy, but for photometry they can be a challenge. They are ideal for the PIN diode photometers, e.g., SSP-3 and SSP-4. For CCD photometry special techniques will be required. Using a telescope will produce saturated images so just a camera lens on a CCD photometry may work. Defocusing helps. The web site describes some ideas for techniques and provides information for both photometry and spectroscopy.
This is an ongoing Project, low stress. Orion is ideally located for most of the civilized world to observe. It is currently in a favorable position at reasonable hours.
If you are interested in contributing, have suggestion, questions or comments, please contact me.phxjeff@hposoft.com
Alert Notice 474: Multiwavelength campaign on delta Ori (Mintaka)
December 14, 2012: An international team of astronomers, including Drs. Tony Moffat (University of Montreal), Michael Corcoran (NASA GSFC), and Noel Richardson (University of Montreal), has requested AAVSO photometry and spectroscopy of delta Ori (Mintaka) in support of their multiwavelength campaign on this hot binary star in Orion's Belt. Satellite observations will include x-ray via NASA's Chandra and precision optical photometry via Canada's MOST.
***Chandra and MOST observations will be carried out
2012 DECEMBER 17 through 2013 JANUARY 7
so coverage is critical throughout this period, and is also needed before and after this period.
*** The astronomers write: "...we make a plea to the astronomical community to obtain simultaneous complementary ground‐based optical observations of the key bright hot binary star delta Orionis (Mintaka, one of the belt stars) in the period between mid December 2012 and early January 2013. Both multi‐band photometry and especially spectroscopy would be most welcome."
They write further: "Massive O‐type stars, though rare, are a primary driver behind the chemical, ionization and pressure evolution of the interstellar medium. Evolution of these stars from main sequence to supernova is driven significantly by stellar‐wind mass loss. Understanding this important connection in individual stars requires a good understanding of the physical stellar parameters.. .combined with detailed understanding of the outflowing wind... Because massive stars are rare, and massive binaries rarer still...dynamical determinations of stellar parameters are only known for a few systems. Our uncertainties regarding mass loss are even worse... Important questions... have not yet been answered." For a more complete description of this campaign, please see the file Mintaka.pdf.
Del Ori (Mintaka, 2.41V, (B‐V) ‐0.40) is the belt star closest to gam Ori (Bellatrix) and bet Ori (Rigel). The del Ori system contains multiple stars and visually is a double star, so be careful not to include the fainter star when making observations.
Photometry: At second magnitude (visual), del Ori is ideally suited to multicolor and near-infrared photoelectric photometry and DSLR photometry, and is a candidate for successful CCD photometry. The extremely small range of this system (2.20-2.32 V) makes visual detection of the brightness changes very difficult.
BVRIJH photometry is requested, ideally 100 data points per night obtained from an average of three measurements per data point. Be sure to include the standard deviation for each set of three measurements (i.e., each data point). Magnitudes should be measured to 0.001, and the JD reported to four places.
Gam Ori (Bellatrix, 1.64V, (B-V) -0.22) should be used as the comparison star.
Spectroscopy: Spectroscopy is strongly encouraged. Observers are requested to use S/N >= 200, R >=10000, integration < 30 min, and range 4000-7000 Å. Observations of Hydrogen alpha (6563 Å) and Helium I (6678 Å) are also requested.
Coordinates for del Ori: RA 05 32 00.40 Dec ‐00:17:56.7 (2000.0)
Charts for del Ori may be created using the AAVSO Variable Star Plotter (www.aavso.org/ vsp). Best results will be obtained by specifying an 'A' scale chart and including no other variables on the chart. Photometrists should use the table accompanying this chart.
Please use the name "DEL ORI" when reporting observations and submit photometric observations to the AAVSO International Database. Spectroscopy should be submitted directly to Dr. Noel Richardson at <richardson@astro. umontreal. ca>.
This campaign is being followed on the AAVSO Observing Campaigns page (www.aavso.org/ observing- campaigns) .
This AAVSO Alert Notice was compiled by Elizabeth O. Waagen.
The aim of this forum is to provide you with lots of extra information about what you can use to take spectra of stars, how to calibrate and get the most information from your spectra, as well as important events happening in the sky and specific projects you can take part in.
SUPERNOVA 2014J IN M82 Stephen J. Fossey, University of London Observatory (ULO), reports the discovery of an apparent supernova (magnitude R = 10.5) in Messier 82 on CCD images obtained by himself (and assisted by students B. Cooke, G. Pollack, M. Wilde, and T. Wright) with a ULO 35-cm Schmidt-Cassegrain telescope at Mill Hill, London, on 2014 Jan. 21.80UT. It is located at: RA 9h 55m 42.14s DEC +69 40' 26.0" (2000), 54" west and 21" south of the galaxy's centre. A pre-discovery image taken by Marco Verstraaten (Twisk, The Netherlands; 30-cm reflector) on Jan. 18.977 UT has been posted at website URL http://www.astropage.nl/nova/PSN_J095542...0_astropage.jpg
Additional CCD magnitudes: K. Itagaki, Japan; 0.50-m reflector; host-galaxy light extracted using previous images; measured by H. Kaneda, Sapporo, Japan; 14.559, [17.0 (Itagaki); 15.571, 14.4 (Itagaki; pre-discovery image); 16.641, 13.9 (Itagaki; pre-discovery image); 17.612, 13.3 (Itagaki; pre-discovery image); 19.618, 12.2 (Itagaki; pre- discovery image); 20.620, 11.9 (Itagaki; pre-discovery image); 21.818, V = 11.7 (Fossey); 22.150, B = 12.96, V = 11.68, R_c = 11.04, I_c = 10.63 (S. Kiyota, Kamagaya, Japan; remotely with an iTelescope 0.43-m astrograph + FLI-PL6303E camera near Mayhill, NM, USA; 22.3, R = 11.0 (Ernesto Guido et. al.,; iTelescope 0.50-m f/6.8 astrograph near Mayhill; position end figures 42s.17, 25".9
G. Dhungana, Southern Methodist University; J. M. Silverman, University of Texas at Austin; J. Vinko, University of Szeged; J. C. Wheeler and G. H. Marion University of Texas at Austin; and R. Kehoe and F. V. Ferrante, Southern Methodist University, on behalf of the ROTSE collaboration, report the pre-discovery detection of PSN J09554214+6940260 = SN 2014J in unfiltered images taken with the 0.45-m ROTSE-IIIb telescope located at McDonald Observatory. Available magnitudes: Jan. 7.340 UT, [14.6; 15.378, 13.5; 17.300, 12.4. They add that, given the brightness of the host galaxy (M82) and the complexity of the field, there is likely some host-galaxy light included in these reported magnitudes due to subtraction artifacts.
Y. Cao, California Institute of Technology; M. M. Kasliwal, Carnegie Institution and Princeton University; A. McKay, University of Texas at Austin; and A. Bradley, Apache Point Observatory, on behalf of the "intermediate Palomar Transient Factory" (iPTF) Collaboration, report that a spectrogram of SN 2014J, obtained on Jan. 22.305 UT with the Dual Imaging Spectrograph on the ARC 3.5-m telescope, indicates that it is a type-Ia supernova with a Si II velocity of 20000 km/s. The best superfit match (cf. website URL http://www.dahowell.com/superfit.html) is to SN 2002bo at -14 days. SN 2014J has a red continuum and deep Na D absorption.
MASTER OT J003059.39+301634.3 - NEW CV IN ANDROMEDA S. Shurpakov et. al. (Moscow State University) and others relay on The Astronomer's Telegram 5774 that the MASTER-Tunka auto-detection system discovered an Optical Transit (OT) source at: RA 00h 30m 59.39s DEC +30 16' 34.3" on 2014 Jan 17.472UT. The OT unfiltered magnitude is 16.1m (limit 18.1m). The OT is seen in 7 images. They have an earlier image with the OT at unfiltered magnitude 18.6m on 2011 Nov 19.634UT (limit 19.5m). The OT has faded by 0.5m (to 16.6m) on images obtained 45 minutes later, on 2014 Jan 17.504UT.
At quiescence it is identical to a blue star: USNO-A2.0 1200-00232738 (00 30 59.46 +30 16 34.9 R=18.2 B=18.7) = USNO-B1.0 1202-0006789 (00 30 59.44 +30 16 34.7 B1=18.96 R1=18.47 B2=19.97 R2=19.21 I=N/A), SDSS J003059.40+301634.4</a> (u=18.27 g=18.07 r=18.03 i=18.03 z=18.03). There is also an UV counterpart GALEX J003059.3+301635</a> (NUV=20.90+/-0.25). There is nothing at this position in 1RXS, 2MASS, GCVS and AAVSO VSX. It was at minimum light on 6 DSS plates and on 39 Palomar/NEAT images on 11 different nights from 2001 Aug. 14 to 2002 Dec. 03. This area of sky in Andromeda was observed by Catalina Sky Survey with 260 detections from June 2005 to Sep. 2013. The object varied from 18.8m to below 20m at quiescence with three outbursts as bright as 16.4m on 2007 Oct. 16 fading to 17.4m on Oct. 21.
Based on the blue colour, amplitude of variability (~3 mag) and historical light curve, MASTER OT J003059.39+301634.3 is a cataclysmic variable, most likely an eclipsing dwarf nova in outburst. Discovery and reference images are available at: http://master.sai.msu.ru/static/OT/003059.39301634.3.png
SUPERNOVA 2013gh IN NGC 7183 (LOSS) 2013gh Aug 08.34 22 02 21.84 -18 55 00.4 18.3 3.2"E 1.2"S David Sand: spectrum Aug 11 reveals type-Ia supernova approximately a week before maximum This was not announced until 2013 Nov 12 (editor)
TX CVN: SYMBIOTIC STAR IN ACTIVE STATE U. Munari et. al., (ANS Collaboration) report on The Astronomer's Telegram 5761 that after the last active phase that began in 2003, the symbiotic star TX CVn has now entered a new active phase. In 2003, TX CVn rose to B=10.5 and there it remained until the end of 2007, when they started monitoring the variable with various ANS Collaboration telescopes in BVRI bands. Their observations show that the star has spent the following 6 years on a steady decline at a rate of 0.084 mag per year in the B band, that took it from B=10.55 on December 2007 to B=11.02 on September 2013, when the star begun a rapid brightening, reaching B=10.65 by early December 2013. Our last measurements for 12 and 13 January 2014 provide B=10.72, B-V=+0.78, V-Rc=+0.62, V-Ic=+1.36.
TX CVn is a enigmatic P=199 days binary star composed by a K5III and what looks like a B9 shell star engulfed by a large external dust shell at a temperature of 450 K. TX CVn remained around B=11.8 for the first half century of its long recorded photometric history. Then, around 1945 it begun a slow and gradual rise in brightness that reached B=10.1 mag in 1967, a level at which the system remained until 1990 when a slow decline begun. On top of this, several outbursts occurred, the largest ones recorded on 1920, 1945, 1952, and 1962, when a peak brightness between B=9.0 and 9.5 mag was always attained.
A low resolution spectrum of TX CVn was obtained on 2014 January 12with the Varese 0.61m telescope equipped with the Multi-Mode Spectrograph. At the shortest wavelengths, the spectrum shows a reinforced B9 shell spectrum, while the K5III continues to dominate in the red. Spectral monitoring with the Asiago 1.22m and 1.82m telescopes shows that over the period 2008-2013 the B9 shell spectrum smoothly declined in intensity, paralleling the decline in B-band brightness. The latest spectrum presents Halpha in moderate emission with a strong P-Cyg profile, blue-shifted by 330 km/s with respect to the emission component.
SUPERNOVA 2013gf (TNTS) 2013gf Nov 06.87 09 05 26.46 +56 24 12.4 18.3 8.4"E 0.6"S J.-J. Zhang: spectrum Nov 7 type-Ia around maximum
SUPERNOVA 2013gg IN UGC 4958 (XINGMING SKY SURVEY) 2013gg Nov 05.87 09 21 08.25 +49 35 33.8 17.9 63.7 "E 34.2"S Discovery images: http://www.xjltp.com/XOSS/XM47ZJ/XM47ZJ.htm D. Milisavljevic: spectrum Nov. 8 reasonable match with the type-IIP event 2006bp at four days after maximum light
Mon Feb 17, 2014 3:18 pm