2019/03/16T20:07:20 から 20:29:30(+30s) まで
30秒*20=10分00秒 ISO3200 長秒時露光のノイズ低減：する t-JST=+20秒
Mewlon210FR/2050mm + LPS-P2 + 60D +EM-200Temma2
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CBAT "Transient Object Followup Reports" 2019 03 14.4227 TCP J05390410+4748030 TCP J05390410+4748030 2019 03 14.4227* 05 39 04.10 +47 48 03.0 11.3 U Aur 9 0 Yuji Nakamura, Kameyama, Mie, Japan, reports his discovery of this TCP (mag 11.3) in Aur on a CCD frame taken on 2019 Mar 14.4227 UT (limiting mag 13.0) using a 135mm F4.0 lens. The object was not shown on a frame taken on 2019 Mar 09.4284 UT (limiting mag 13.0). There is a 19.2 mag star USNO-A2.0 1350-06029095 on this position. 2019 03 14.65 Gaia DR2 position end figures for the abovementioned star USNO-A2.0 1350-06029095 are 04.103s, 00.71" (equinox J2000.0, epoch 2015.5; Gmag. 19.67, parallax 3.0826 ± 0.5239 mas, distance ~0.3 kpc). Other designations are USNO-B1.0 1378-0184085, GSC2.3 NAO9008900, PSO J053904.098+474800.708, GALEX J053904.0+474800, AllWISE J053904.08+474759.9, WDJ053904.11+474800.65WDJ053904.11+474800.65. The transient is probably a dwarf nova outburst with an amplitude of about 8 magnitudes (WZ Sge type?). Spectroscopy as well as multiband and time-resolved photometry are strongly recommended. --- Patrick Schmeer (Saarbrucken-Bischmisheim, Germany) 2019 3 15.1726 Photometry results were V=11.80 and Ic=11.80 with 0.61-m f/6.5 CDK astrograph + FLI PL09000 CCD at iTelescope.NET (Sierra Remote Observatory - Auberry, California. USA). Position end figures were 04.10 and 1.0. http://meineko.sakura.ne.jp/ccd/TCP_J05390410+4748030.jpg Seiichiro Kiyota (Kamagaya, Japan) 2019 03 15.759 P. Berardi (ARAS) and Giuseppe Di Carlo, L'Aquila, Italy, obtained a low-resolution spectrum of this transient on 2019 Mar 15, 18:13 UT. Observation was performed at Bellavista Observatory (MPC code C93), using 0.23 m SCT telescope and Lhires III spectrograph configured for low resolving power (4200-7000A, 10A res.). The spectrum shows a blue continuum, emission of H-alpha line, a narrow component in a broad absorption for H-beta line, emission of CIII/NIII 4640 blend and several He I/II emission lines. All that suggests that the transient is a dwarf nova, WZ Sge type. Spectral profile is available here: http://quasar.teoth.it/html/spectra/tcpj05390410+4748030_BD.png |
2019年03月16日
