We examined a random star field near to galactic band using Exoplanet Blue Blocking filter (The spectrum of the Astrodon ExoPlanet-BB filter is shown Below). It blocks UV and blue light. It starts transmitting light near 500 nm, corresponding to the shape of the conventional V-band filter and continues to transmit light into the near-infrared.
The purpose of using this filter was to achieve the best possible focus at red end. The 40 sub frames of 120 seconds were taken using PRiSMv10. The image stacked and photometrically calibrated using star catalog ATLAS and Tycho8.0. We achieved the best possible average magnitudes at V band (conversion) to +21.50
Image: Object: Random Star Field DATE-OBS: 2021-04-18T21:28:25 EXPTIME(Seconds): *B/*V/*R/*I/*g’2/*r’2/*i’2/*z’2/4800ExBB SUBFRMS: *B/*V/*R/*I/*g’2/*r’2/*i’2/*z’2/40ExBB OBJCTRA: 18 19 30.15 OBJCTDEC: +09 28 07.1 Instrument: Astrometry Catalog: ATLAS: Y, UCAC4: N, GAIAEDR3: N Photometry Catalog: : UCAC4: N, APASS: N, ATLAS: Y Johnson/Bessel: (B): *.*, (V): *.*, (R): *.*, (I): *.* Sloan: g’2: *.*, r2: *.*, i’2: *.*, z’2: *.* CCD: ATIK-383L+ FILTERS: Sloan: u’2: N,g’2: N,r’2: N,i’2: N,z’2: N, ExBB: Y Johnson/Bessel: U: N,B: N,V: N,R: N,I: N, TELESCOPE: C11, 1623.0mm PRiSMv10, Tycho8.0 Site: ORIGIN: Cepheid Observatory, India, Vorion Scientific, India SITELAT: +24:55:00:00 SITELONG:+75:33:58:99 Observers: K.V Measures: S.M, B.K, V.A. Remark: Sky Clear, End
Electronic Telegram No. 4955 Central Bureau for Astronomical Telegrams Mailing address: Hoffman Lab 209; Harvard University; 20 Oxford St.; Cambridge, MA 02138; U.S.A. e-mail: cbatiau at eps.harvard.edu (alternate cbat at iau.org) URL http://www.cbat.eps.harvard.edu/index.html Prepared using the Tamkin Foundation Computer Network
V1710 SCORPII = NOVA SCORPII 2021 = PNV J17091000-3730500 Paul Camilleri, Katherine, Northern Territory, Australia, reports his discovery of an apparent nova (mag 9.5) on three 5-s exposures taken on Apr. 12.7625 UT with a Nikon D3200 digital SLR camera (+ 85-mm-f.l. f/2 lens), noting the variable to have an orange color; the approximate position was given as R.A. = 17h09m50s, -37d30’50” (equinox J2000.0). The variable was given the provisional designation PNV J17091000-3730500 automatically when it was posted to the Central Bureau’s TOCP webpage. R. Fidrich, Budapest, Hungary, provides position end figures 08s.11, 40″.9 measured on a B-band CCD image obtained on Apr. 12.814 with an iTelescope 0.50-m f/6.8 reflector located at Siding Spring, NSW, Australia. F. Kugel, Banon, France, measured position end figures 08s.32, 42″.6 from three stacked 30-s CCD images taken with a 195-mm-f.l. f/2.8 lens on Apr. 13.12. A. Pearce, Nedlands, W. Australia, provides position end figures 08s.10, 40″.9 from a CCD image obtained remotely on Apr. 13.632 with a 0.43-m f/6.8 reflector located at Siding Spring (reference stars from the Gaia DR2 catalogue). Additional digital-image magnitudes (unfiltered unless noted otherwise) that have been reported for PNV J17091000-3730500: Apr. 11.395 UT, [16.8 (All-Sky Automated Survey for Supernovae; communicated by P. Schmeer, Saarbruecken-Bischmisheim, Germany); 11.682, [13.8 (R. McNaught, Coonabarabran, NSW, Australia; 59-s exposure with Canon 6D camera + 135-mm-f.l. f/2.8 lens); 11.758, [12 (Camilleri); 11.794, [13.5 (McNaught); 12.168, g = 11.1 (ASAS-SN; independent discovery reported by Schmeer; position end figures 08s.11, 40″.4); 12.408, g = 10.4 (ASAS-SN; Schmeer); 12.55, 9.5 (R. Kaufman, Bright, Vic., Australia; green channel approximating V band, Canon 800D camera + 200-mm-f.l. lens; image posted via the following URL https://tinyurl.com/4t5akzyy); 12.583, 9.6 (McNaught); 12.687, 9.5 (McNaught); 12.796, 9.4 (McNaught); 12.814, B = 10.64 (Fidrich; the variable was very red, with B-V being at least +1.5); 12.955, R = 8.03 (V. Agnihotri, Kota, Rajasthan, India; communicated via E. O. Waagen, AAVSO); 12.965, I = 7.09 (Agnihotri); 12.972, V = 8.84 (Agnihotri); 13.12, 8.9 (Kugel); 13.372, B = 9.71 (J. Backman, Lappeenranta, Finland; via Waagen); 13.422, B = 10.05 (J.-F. Hambsch, Mol, Belgium; via Waagen); 13.423, I = 6.74 (Hambsch); 13.424, V = 8.69 (Hambsch); 13.632, V = 8.53 (Pearce); 13.633, B = 10.32 (Pearce); 13.634, I = 6.58 (Pearce); 13.787, 8.5 (F. Romanov, Yuzhno-Morskoy, Nakhodka, Russia; from five stacked 5-s exposures taken with a Canon EOS 60D camera + 135-mm-f.l. f/5.6 lens at ISO 6400 with a hazy sky; image posted at website URL https://www.flickr.com/photos/filipp-romanov/51114244018). Visual magnitude estimates for PNV J17091000-3730500: Apr. 13.068 UT, 8.8 (A. Amorim, Florianopolis, Brazil; via Waagen); 13.128, 8.9 (L. Araujo, Pelotas, Brazil; via Waagen); 13.342, 8.7 (Amorim); 13.715, 8.8 (C. Wyatt, Walcha, NSW, Australia; via Waagen); 13.732, 8.8 (Pearce). Waagen also informs the Bureau that Joshi et al. have reported that their spectroscopy obtained on Apr. 12.916 UT with the Mt. Abu PRL 1.2-m telescope (range 440-900 nm, resolutions about 500 and 2000) show this to be an “Fe II”- type of classical nova caught early in its outburst, with H-alpha, H-beta, Fe II, and O I lines showing P-Cyg profiles on a red continuum (details are given at website URL https://www.astronomerstelegram.org/?read=14544). E. Kazarovets informs the Central Bureau that the permanent GCVS designation V1710 Sco has been given to this nova.
NOTE: These ‘Central Bureau Electronic Telegrams’ are sometimes superseded by text appearing later in the printed IAU Circulars.