- vsnet-campaign-nova - ooruri.kusastro.kyoto-u.ac.jp

[vsnet-campaign-nova 2289] ATLAS22beux
by Taichi Kato 21 Sep '22

21 Sep '22

ATLAS22beux https://www.aavso.org/vsx/index.php?view=detail.top&oid=2344694 There is a GALEX counterpart. 062908.682 -712937.92 (2000.0) GALEX_DR5_6385763624932083805 NUV=21.265(0.381) FUV=21.777(0.450)

1 0

[vsnet-campaign-nova 2288] Re: AT2022sfe: likely highly reddened nova
by Taichi Kato 30 Aug '22

30 Aug '22

Re: AT2022sfe: likely highly reddened nova Accoring to > https://www.wis-tns.org/object/2022sfe The Gaia object appears to be the northern component of the pair. 200029.264 +345308.30 (2000.0) Gaia_EDR3_2059315910815578496 plx=-(-) dismod=- pmra=-(-) pmdec=-(-) G=21.008 BP=21.178 RP=19.371 The location 20:00:29.256 +34:53:09.14 is very slightly different from this location. A faint object not in Gaia may be outbursting now.

1 0

[vsnet-campaign-nova 2287] AT2022sfe: likely highly reddened nova
by Taichi Kato 30 Aug '22

30 Aug '22

AT2022sfe: likely highly reddened nova Moriyama-san has pointed out the red color. YYYYMMDD(UT) mag observer 20220827.5919 15.53C (Masayuki Moriyama) 20220828.6528 15.34C (Masayuki Moriyama) 20220828.6559 14.99Rc (Masayuki Moriyama) 20220828.6576 13.51Ic (Masayuki Moriyama) 20220828.6593 <16.39B (Masayuki Moriyama) 20220828.6638 16.92:V (Masayuki Moriyama) See: https://www.wis-tns.org/object/2022sfe The object is located very close to the northern component of a close pair in the PS1 image. The Gaia object appears to be the southern component of the pair. 200029.264 +345308.30 (2000.0) Gaia_EDR3_2059315910815578496 plx=-(-) dismod=- pmra=-(-) pmdec=-(-) G=21.008 BP=21.178 RP=19.371 The outbursting object may not be related to them.

1 0

[vsnet-campaign-nova 2286] Gaia22doh
by Taichi Kato 29 Aug '22

29 Aug '22

Gaia22doh Likely reddened nova. http://gsaweb.ast.cam.ac.uk/alerts/alert/Gaia22doh/ Gaia22doh AT2022sie 2022-08-26 05:03:03 235.24023 -54.59284 16.89 unknown 2022-08-27 20:49:03 Apparently hostless bright red transient

1 0

[vsnet-campaign-nova 2284] Gaia22alz (ATel)
by Taichi Kato 02 May '22

02 May '22

Gaia22alz (ATel) Slowest classical nova ever observed and early premaximum spectra were obtained. The Astronomer's Telegram http://www.astronomerstelegram.org ============================================================================== ATEL #15355 ATEL #15355 Title: Intriguing developments in the slowly rising Galactic optical transient Gaia22alz (AT2022bpq) Author: E. Aydi, K. V. Sokolovsky, J. Strader, L. Chomiuk, A. Kawash (MSU), J. Brink, D. A. H. Buckley (SAAO/UCT), M. Orio (UoW/INAF), J. Mikolajewska (NCAC), K. Z. Stanek, C. S. Kochanek (OSU), and B. J. Shappee (Univ. of Hawaii) Queries: aydielia(a)msu.edu Posted: 29 Apr 2022; 21:18 UT Subjects:Optical, Ultra-Violet, X-ray, Binary, Cataclysmic Variable, Nova, Star, Transient, Variables We report on multi-wavelength follow up of the slowly rising Galactic optical transient Gaia22alz (AT2022bpq), which was discovered by Gaia on 2022-02-04.2UT (https://www.wis-tns.org/object/2022bpq) Earlier follow up by Brink et al. (ATel #15270) on 2022-03-11 reported optical spectra dominated by emission lines of Balmer, He II, He I, and C IV, characterized by a FWHM of around 400-500 km/s. Based on photometry from the All-Sky Automated Survey for SNe (ASAS-SN; Shappee et al. 2014, ApJ, 788, 48S and Kochanek et al. 2017PASP, 129, 4502) the transient, which started around 2022-01-25, is still rising slowly and reached a magnitude g = 13.1 on 2022-04-29 (see below a link to the latest ASAS-SN light curve). In archival data from the Dark Energy Camera Plane Survey (DECaPS; Schlafly 2018, ApJs 234, 39) the source has a pre-outburst magnitude g = 18.9, implying a current outburst amplitude of 5.8 mag. We have obtained a series of low-, medium-, and high-resolution optical spectra on 2022-03-15, 04-03, 04-09, 04-10, 04-14, and 04-21 using the Goodman spectrograph (Clemens et al. 2004, SPIE, 5492, 331) on the 4.1-m SOAR telescope (Cerro Pachon, Chile) and the High Resolution Spectrograph (HRS; Crause et al. 2014, Proc. SPIE, 91476) mounted on the 11-m Southern African Large Telescope as part of the SALT Large Science Program on Transients. The spectrum obtained on 2022-03-15 showed similar features to the ones reported in Brink et al. (ATel #15270). However, from 2022-04-03 onwards, the spectra showed dramatic changes with the He II and C IV emission lines fading considerably, and the Balmer and He I lines developing prominent P Cygni absorption profiles at blueshifted velocities of 1700-1800 km/s, indicating the presence of an optically thick outflow. The spectra at this stage resemble those of classical novae before optical peak, but further follow up are required to determine the nature of this event. The slowly rising light curve and the spectral changes make this an interesting transient and multi-wavelength follow up are highly encouraged. Based on the absorption by diffuse interstellar bands (DIBs) and the empirical relations from Friedman et al. 2011 (ApJ 727, 33), we derive E(B-V) = 1.5 mag and Av = 4.65 mag, assuming Rv = 3.1. This is higher than the estimate of Av = 3.472 mag from the Schlafly et al. (2011, ApJ 737, 1035) Galactic reddening maps. The Neil Gehrels Swift Observatory observed Gaia22alz for 0.7ks on 2022-04-20.53 (JD 2459690.03). Swift/XRT detected no X-ray source at the position of the nova with an upper limit of 0.003 +/-0.002 cts/s. Assuming emission by a kT= 2 keV thermal plasma and an HI column density of 76.10x10^20 cm^-2 (Kalberla et al. 2005 A&A, 440, 775) this translates to an unabsorbed 0.3-10.0 keV flux limit of 7x10^-13 ergs/cm^2/s. An ultraviolet source is detected at the position of the transient by Swift/UVOT with UVW2 magnitude = 15.01 +\- 0.03 (Vega system). The ASAS-SN sky patrol light curve can be found here: https://asas-sn.osu.edu/sky-patrol/coordinate/cef95f4e-66e7-4a2b-ad65-608ca… This ATel is based on observations obtained at the Southern Astrophysical Research (SOAR) telescope, which is a joint project of MCTIC/LNA, the U.S. NSF's NOAO, UNC, and MSU. We also acknowledge ESA Gaia, DPAC and the Photometric Science Alerts Team (<a href="http://gsaweb.ast.cam.ac.uk/alerts">http://gsaweb.ast.cam.ac.uk/alerts</a>). We thank the Neil Gehrels Swift Observatory team and PI, Brad Cenko, for rapid scheduling these ToO observations. The Dark Energy Camera Plane Survey (DECaPS; NOAO Proposal ID 2016A-0323 and 2016B-0279, PI: D. Finkbeiner) includes data obtained at the Blanco telescope, Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory (NOAO). ------------------------------------------------------------------------------ Password Certification: Elias Aydi (aydielia(a)msu.edu) https://www.astronomerstelegram.org/?read=15355 ==============================================================================

2 1

[vsnet-campaign-nova 2283] ASASSN-22an: possible nova
by Taichi Kato 11 Jan '22

11 Jan '22

ASASSN-22an: possible nova ASASSN-22an --- ------- 15:24:49.56 -57:39:52.7 2022-01-8.34 15.28 SDSS DSS VIZIER ------- possible Nova, very high extinction region, matches to GAIA DR2 G=19.6, g>17.6 on 2021-10-05.74, g=14.6 on 2021-10-08.98, g=15.6 on 2022-01-08.34 ASASSN-22an 20211005.74 <176g ASN ASASSN-22an 20211008.98 146g ASN ASASSN-22an 20210108.34 156g ASN

1 0

[vsnet-campaign-nova 2282] V606 Vul rapid fading: more complete data set
by Taichi Kato 09 Nov '21

09 Nov '21

V606 Vul rapid fading: more complete data set YYYYMMDD(UT) mag observer 20211031.506 119 (Hiroyuki Maehara) 20211031.7556 123 (Eddy Muyllaert) 20211101.3590 10.878Rc (Yasuo Sano) 20211101.3595 12.989B (Yasuo Sano) 20211101.3597 12.113V (Yasuo Sano) 20211101.3603 10.802C (Yasuo Sano) 20211101.6277 122V (Masayuki Moriyama) 20211101.6318 118C (Masayuki Moriyama) 20211101.7514 120 (Eddy Muyllaert) 20211101.962 119 (Gary Poyner) 20211102.433 128 (Takuichiro Onishi) 20211102.474 124 (Yoshiyasu Sato) 20211102.6065 12.73V (Masayuki Moriyama) 20211102.7576 124 (Eddy Muyllaert) 20211102.850 124 (Gary Poyner) 20211103.431 122 (Takuichiro Onishi) 20211103.494 124 (Yoshiyasu Sato) 20211103.6018 12.20V (Masayuki Moriyama) 20211104.408 132 (Takuichiro Onishi) 20211104.5663 136V (Masayuki Moriyama) 20211104.750 124 (Gary Poyner) 20211105.3628 10.930Rc (Yasuo Sano) 20211105.428 122 (Yoshiyasu Sato) 20211105.4457 12.979B (Yasuo Sano) 20211105.4459 12.169V (Yasuo Sano) 20211105.4464 11.025C (Yasuo Sano) 20211105.7514 123 (Eddy Muyllaert) 20211106.4210 13.09V (Minoru Sato) 20211106.5764 13.69V (Masayuki Moriyama) 20211106.5781 12.58Rc (Masayuki Moriyama) 20211106.5796 11.90Ic (Masayuki Moriyama) 20211106.5991 <14.51B (Masayuki Moriyama) 20211107.3990 15.152B (Yasuo Sano) 20211107.3998 12.872C (Yasuo Sano) 20211107.4003 14.282V (Yasuo Sano) 20211107.4006 12.565Rc (Yasuo Sano) 20211107.419 <143 (Takuichiro Onishi) 20211107.492 143 (Hiroyuki Maehara)

1 0

[vsnet-campaign-nova 2281] Re: V606 Vul rapid fading
by Taichi Kato 08 Nov '21

08 Nov '21

Re: V606 Vul rapid fading 20211104.408 132 (Takuichiro Onishi) 20211104.750 124 (Gary Poyner) 20211105.7514 123 (Eddy Muyllaert) 20211107.492 143 (Hiroyuki Maehara) The object had already faded to V=13.6 on Nov. 4.

1 0

[vsnet-campaign-nova 2280] V606 Vul rapid fading
by Taichi Kato 08 Nov '21

08 Nov '21

V606 Vul rapid fading YYYYMMDD(UT) mag observer 20211101.6277 122V (Masayuki Moriyama) 20211101.6318 118C (Masayuki Moriyama) 20211101.7514 120 (Eddy Muyllaert) 20211101.962 119 (Gary Poyner) 20211102.433 128 (Takuichiro Onishi) 20211102.474 124 (Yoshiyasu Sato) 20211102.6065 12.73V (Masayuki Moriyama) 20211102.7576 124 (Eddy Muyllaert) 20211102.850 124 (Gary Poyner) 20211103.431 122 (Takuichiro Onishi) 20211103.494 124 (Yoshiyasu Sato) 20211103.6018 12.20V (Masayuki Moriyama) 20211104.408 132 (Takuichiro Onishi) 20211104.750 124 (Gary Poyner) 20211105.7514 123 (Eddy Muyllaert) 20211107.492 143 (Hiroyuki Maehara)

1 0

[vsnet-campaign-nova 2279]V2109 Oph (1969 nova) undergoing a dwarf-nova outburst
by Taichi Kato 27 Aug '21

27 Aug '21

V2109 Oph (1969 nova) undergoing a dwarf-nova outburst http://gsaweb.ast.cam.ac.uk/alerts/alert/Gaia21dza/ ZTF data: Slowly rising. The orbital period appears to be long, which would explain why dwarf-nova outbursts occur less than 50 years after the nova eruption. YYYYMMDD(UT) mag observer 20210522.6098 <161C (Masayuki Moriyama) 20210529.5639 <162C (Masayuki Moriyama) 20210708.2728 18.919zg (Zwicky Transient Facility Lasair (Masci+ 2019)) 20210711.2099 18.779zg (Zwicky Transient Facility Lasair (Masci+ 2019)) 20210717.2314 18.482zg (Zwicky Transient Facility Lasair (Masci+ 2019)) 20210728.2110 17.740zg (Zwicky Transient Facility Lasair (Masci+ 2019)) 20210804.1900 17.560zg (Zwicky Transient Facility Lasair (Masci+ 2019)) 20210813.1726 17.119zg (Zwicky Transient Facility Lasair (Masci+ 2019)) 20210813.1896 16.475zr (Zwicky Transient Facility Lasair (Masci+ 2019)) 20210815.2105 16.839zg (Zwicky Transient Facility Lasair (Masci+ 2019)) 20210821.1747 17.021zg (Zwicky Transient Facility Lasair (Masci+ 2019))

1 0