Exo-Planet Observations, Class confirmed
HAT-P-12b
Imaged/Calibration/Image solve: PRiSM v11
Photometry and Data Fitting: HOPS 2.5.6/Platform: Python 3.7.6
C11/F5.12+CCD
Cepheid Observatory India
Vorion Scientific Observatory India
Exo-Planet Observations, Class confirmed Wasp-65b Imaged/Calibration/Image solve: PRiSM v11Photometry and Data Fitting: HOPS 2.5.6/Platform: Python 3.7.6C11/F5.12+CCDCepheid Observatory IndiaVorion Scientific Observatory India
Exo-Planet Observations, Class confirmed Wasp-104b Imaged/Calibration/Image solve: PRiSM v11Photometry and Data Fitting: HOPS 2.5.6/Platform: Python 3.7.6C11/F5.12+CCDSome of data could not be used for Wasp-104b during transit due to bad sky conditions.Cepheid Observatory IndiaVorion Scientific Observatory India
SN 2020jfo: Astrometry/Photometry (V/R/I)
R/ MAGNITUDE= 15.00, RA(2000) = 12h21m50.475s, DEC(2000)= +04°28’54.26”
V/ MAGNITUDE= 14.84, RA(2000) = 12h21m50.476s, DEC(2000)= +04°28’54.48”
I/ MAGNITUDE= 14.88, RA(2000) = 12h21m50.482s, DEC(2000)= +04°28’54.35”
DATE-OBS= 2020-05-07T14:54:40.87
SWCREATE= PRISMv10/ UCAC4
ORIGIN = Cepheid Observatory
OBSERVER= Agnihotri V K, K Bikash, Mahawar S, Vora K
INSTRUME= ARTEMIS CCD ATIK-383L
TELESCOP= C8/1286.0mm/208.0mm
Cepheid Observatory India
Vorion Scientific Observatory India
Adding Multiband Photometry data TCP J15472959-0532144.
Astrometry: Catalog UCAC4, J2000
RA= 15h47m29.84s DEC= -05°32’17.94”
UT 30.988 R MAGNITUDE= 13.61 ±0.10
UT 30.991 I MAGNITUDE= 13.71 ±0.10
UT 30.993 V MAGNITUDE= 13.51 ±0.09
UT 30.998 B MAGNITUDE= 13.63 ±0.23
Tele: 0.28m Schmidt–Cassegrain+CCD +Bessell BVRI
PRiSMv10
http://www.cbat.eps.harvard.edu/…/J15472959-0532144.html
Imaged: K. Vora, Vorion Scientific Observatory, AHD, India
Measured: V.K. Agnihotri, Cepheid’s Observatory RBT, India
WASP-12b, Class Exoplanet Confirmed.
Mid-time: 2456176.668258 ± 7.8e-05 BJDTDB
Period: 1.0914203 ± 1.4e-07 days
Rband Depth*: 17.35 mmag
Duration*:n3.02 hours
Teff: 6300 K, Log(g): 4.11 cm/s2, Fe/H: 0.3 dex
Rp/Rs: 0.11761006, a/Rs: 2.981
AstroImageJ 3.3.1
Cepheid Observatory India
Vorion Scientific Observatory India
Comet C/2019Y4 ATLAS: V/R Photometry.
The spectroscopy of gas and terrestrial planets
Spectrum: TCP J04291884+4354232 (Classical Nova)
C11/f5.7/Alpy600/PRiSMv10/RSpec/Magicplotpro/Originpro-2021
We saw P-cygni profile in H beta and Halpha.
After posting result related to Nebular Density Ratio of M42 “Orion Nebula” The results for Nebular Density Ratio without Interstellar Redding correction were c(Hb) = 0.0:
Ha/Hb = 5.17
Hy/Hb = 0.35
OIII5007/OIII4959 = 3.0
We have corrected data for interstellar extinction using formula:
c(Hb)= 3.08Xlog(I(Ha)-7.55, Ic=IoX10^(c*f).
We found c(Hb) equal to 0.81. In continuation, the paper said the IS extinction in between 0.0 to 1.6 for M42, but most of the places it is near to value 0.8.
The results for Nebular Density Ratio with Interstellar Redding correction c(Hb) = 0.81:
Ha/Hb = 2.79
Hy/Hb = 0.49
OIII5007/OIII4959 = 2.92
See paper link https://iopscience.iop.org/article/10.1086/301429/fulltext/
The corrected data are shown by dotted points:
If We follow paper given in link https://www.aanda.org/…/2011/01/aa14464-10/aa14464-10.html
and use IS extinction formula given by then
The results for Nebular Density Ratio with Interstellar Redding correction c(Hb) = 0.73:
Ha/Hb = 2.97
Hy/Hb = 0.48
OIII5007/OIII4959 = 2.93
Doing this exercise We guess, the slit was exposed in a place where IS extinction was in between 0.81 to 0.73.
