Photometry: K2-295b

cepheids

Exo-Planet, Class confirmed:
K2-295b
Imaged/Calibration/Image solve:
PRiSM v11
Photometry and Data Fitting:
HOPS 3.1.2/Platform: Python 3.9
Instrument:
CCD: Atik383L+ (KAF8300M)
FILTERS: Luminance
TELESCOPE: C11, 1670.0 mm
Site:
ORIGIN: Cepheid Observatory India
SITELAT: +24:55:00:00
SITELONG:+75:33:58:99
Observers:
Cepheid Observatory India, VS Observatory India
Remark:
Sky Clear

Results
Rp/Rs = 0.1443 ± 0.0059 (expected: 0.1304 ± 0.0014)
O-C = -0.84 ± 2.16 minutes
Diagnostics
Transit SNR = 12.28 (good:≥5, acceptable:≥3)
(strong detection of the transit)
Rp/Rs drift = 2.29σ (good:≤2, acceptable:≤3)
(Rp/Rs in marginal agreement with the literature)
AutoCorrelation = 0.274 (good:≤0.33, acceptable:≤0.404)
(no systematics in the data)
Shapiro = 0.009 (good:≤0.035, acceptable:≤0.059)
(few or no outliers in the data)

Photometry: WASP-44b

cepheids

Exo-Planet, Class confirmed:
WASP-44b
Imaged/Calibration/Image solve:
PRiSM v11
Photometry and Data Fitting:
HOPS 3.1.2/Platform: Python 3.9
Instrument:
CCD: Atik383L+ (KAF8300M)
FILTERS: Luminance
TELESCOPE: C11, 1670.0 mm
Site:
ORIGIN: Cepheid Observatory India
SITELAT: +24:55:00:00
SITELONG:+75:33:58:99
Observers:
Cepheid Observatory India, VS Observatory India
Remark:
Sky Clear

Results
Rp/Rs = 0.1238 ± 0.0042 (expected: 0.126 ± 0.003)
O-C = 0.6 ± 1.32 minutes
Quality check
Residuals STD (Standard Deviation) = 3.695 ‰
Based on your past observations, this is better than expected (5.734 ‰).
Diagnostics
Step 1: Transit SNR = 14.8
Transit SNR is good (strong detection of the transit)
Step 2: Rp/Rs drift = -0.43σ
The Rp/Rs drift is good (Rp/Rs in good agreement with the literature)
Step 3: AutoCorrelation = 0.185
The AutoCorrelation is good (no systematics in the data)
Step 4: Shapiro test = 0.019
The Shapiro test is good (few or no outliers in the data)

Photometry: TOI-3714b

cepheids

Exo-Planet, Class confirmed:
TOI-3714b
Imaged/Calibration/Image solve:
PRiSMv11
Photometry and Data Fitting:
HOPS 3.1.2/Platform: Python 3.9
Instrument:
CCD: Atik383L+ (KAF8300M)
FILTERS: Luminance
TELESCOPE: C11, 1670.0 mm
Site:
ORIGIN: Cepheid Observatory India
SITELAT: +24:55:00:00
SITELONG:+75:33:58:99
Observers:
Cepheid Observatory India, VS Observatory India
Remark:
Sky Clear

Results
Rp/Rs = 0.205 ± 0.01 (expected: 0.204 ± 0.003)
O-C = -3.62 ± 1.28 minutes
Quality check
Residuals STD (Standard Deviation) = 13.867 ‰
Diagnostics
Step 1: Transit SNR = 10.3
Transit SNR is good (strong detection of the transit)
Step 2: Rp/Rs drift = 0.1σ
The Rp/Rs drift is good (Rp/Rs in good agreement with the literature)
Step 3: Auto Correlation = 0.304
The Auto Correlation is good (no systematics in the data)
Step 4: Shapiro test = 0.028
The Shapiro test is good (few or no outliers in the data)

Photometry: WASP-177b

cepheids

Exo-Planet, Class confirmed:
WASP-177b
Imaged/Calibration/Image solve:
PRiSMv11
Photometry and Data Fitting:
HOPS 3.1.2/Platform: Python 3.9
Instrument:
CCD: Atik383L+ (KAF8300M)
FILTERS: Luminance
TELESCOPE: C11, 1670.0 mm
Site:
ORIGIN: Cepheid Observatory India
SITELAT: +24:55:00:00
SITELONG:+75:33:58:99
Observers:
Cepheid Observatory India, VS Observatory India
Remark:
Sky Clear

Results
Rp/Rs = 0.139 ± 0.012 (expected: 0.136 ± 0.0129)
O-C = -0.09 ± 3.46 minutes
Quality check
Residuals STD (Standard Deviation) = 3.816 ‰
Based on your past observations, this is better than expected (3.82 ‰).
Diagnostics
Step 1: Transit SNR = 6.45
Transit SNR is good (strong detection of the transit)
Step 2: Rp/Rs drift = 0.17σ
The Rp/Rs drift is good (Rp/Rs in good agreement with the literature)
Step 3: Auto Correlation = 0.46
Step 4: Shapiro test = 0.012
The Shapiro test is good (few or no outliers in the data)

Photometry: HAT-P-25b

cepheids

Exo-Planet, Class confirmed:
HAT-P-25b
Imaged/Calibration/Image solve:
PRiSMv11
Photometry and Data Fitting:
HOPS 3.1.2/Platform: Python 3.9
Instrument:
CCD: Atik383L+ (KAF8300M)
FILTERS: Luminance
TELESCOPE: C11, 1670.0 mm
Site:
ORIGIN: Cepheid Observatory India
SITELAT: +24:55:00:00
SITELONG:+75:33:58:99
Observers:
Cepheid Observatory India, VS Observatory India
Remark:
Sky Clear

Results
Rp/Rs = 0.1231 ± 0.0042 (expected: 0.1269 ± 0.0011)
O-C = -2.81 ± 1.87 minutes
Quality check
Residuals STD (Standard Deviation) = 4.698 ‰
Based on your past observations, this is better than expected (6.164 ‰).
Diagnostics
Step 1: Transit SNR = 14.7
Transit SNR is good (strong detection of the transit)!
Step 2: Rp/Rs drift = -0.88σ
The Rp/Rs drift is good (Rp/Rs in good agreement with the literature)!
Step 3: Auto Correlation = 0.204
The Auto Correlation is good (no systematics in the data)
Step 4: Shapiro test = 0.006
The Shapiro test is good (few or no outliers in the data)

Photometry: TrES-5b

cepheids

Exo-Planet, Class confirmed:
TrES-5b
Imaged/Calibration/Image solve:
PRiSM v11
Photometry and Data Fitting:
HOPS 3.1.2/Platform: Python 3.9
Instrument:
CCD: Atik383L+ (KAF8300M)
FILTERS: Clear
TELESCOPE: C11, 1670.0 mm
Site:
ORIGIN: Cepheid Observatory India
SITELAT: +24:55:00:00
SITELONG:+75:33:58:99
Observers:
Cepheid Observatory India, VS Observatory India
Remark:
Sky Clear

Results
Rp/Rs = 0.1361 ± 0.0049 (expected: 0.142 ± 0.0009)
O-C = 0.8 ± 1.87 minutes

Quality check
Residuals STD (Standard Deviation) = 5.915 ‰
Based on your past observations, this is better than expected (7.704 ‰). Great!

Diagnostics
Step 1: Transit SNR = 13.97
Transit SNR is good (strong detection of the transit)!
Step 2: Rp/Rs drift = -1.18σ
The Rp/Rs drift is good (Rp/Rs in good agreement with the literature)!
Step 3: Auto Correlation = 0.151
The Auto Correlation is good (no systematics in the data)!
Step 4: Shapiro test = 0.005
The Shapiro test is good (few or no outliers in the data)!

Photometry: RR Lyrae/V* RR Lyr

cepheids

RR Lyrae variables are old, low-mass, radially pulsating stars with periods in the range between 0.2 and 1 day. They are a numerous class of variable stars that populate galactic halos, thick disks and globular clusters. In the H-R diagram, RR Lyrae stars can be found in the narrow region where the horizontal branch intersects the pulsational instability strip. Their relatively small range of absolute mean magnitudes (because they lie on the horizontal branch) makes them important distance indicators in both our own Galaxy and those nearby. RR Lyrae stars are also excellent tracers of the chemical and dynamical properties of the oldest observable population of stars, so they give us insight into the earliest history of galaxies. Taking into account the pulsation modes, RR Lyrae stars can be divided into fundamental-mode (commonly referred to as RRab stars, sometimes called RR0 stars), first-overtone (RRc or RR1 stars) and double-mode (RRd or RR01 stars) pulsators. The existence of second-overtone pulsators among RR Lyrae variables (RRe or RR2 stars) is a matter of controversy. https://ogle.astrouw.edu.pl/atlas/RR_Lyr.html

Object: RR Lyrae
DATE-OBS: 2023-10-04T14:24:04.5960 + 2 Days
EXPTIME(Hrs): 5.64
SUBFRMS: 451
OBJCTRA: 19 25 27.872
OBJCTDEC: +42 46 59.05
Binning: 1 X 1
Plate Scale: 1.53″ /Pixel
Orientation: North UP/ East Left
Catalogs & Filter Magnitude Results:
Astrometry Catalog: ATLAS
Photometry Catalog: ATLAS
Imaging Filter: CLEAR
Photometry Mag: +7.6 R
Instruments:
CCD: ICX694M (4.5µm x 4.5µm)
TELESCOPE: 132MM APO, 610mm
PRiSMv11, Tycho10.8.4, Maxim DL
Site:
ORIGIN: Cepheid Observatory, India
SITELAT: +24:55:00:00
SITELONG:+75:33:58:99
Observers:
Cepheid Observatory
Remark:
Sky Clear

Note: The observations is done partially for 3 days, as object was visible for few hours in every night. The RR Lyrae have period of 0.56689 days and some of portions of possible maxima and minima covered. The exercise is done for learning and interest. https://browse.arxiv.org/pdf/astro-ph/0601432.pdf

Comet 12P/Pons-Brooks

cepheids

Image Info:
Object: 12P/Pons-Brooks
DATE-OBS: 2023 10 01.60177
EXPTIME(mins): 54
SUBFRMS: 27
OBJCTRA: 17 20 14.43
OBJCTDEC: 46 45 46.2
Binning: 1 X 1
Plate Scale: 1.53″ /Pixel
Orientation: North UP/ East Left
Catalogs & Filter Magnitude Results:
Astrometry Catalog: ATLAS
Photometry Catalog: ATLAS
Imaging Filter: CLEAR
Photometry Mag: +14.9 V
Instruments:
CCD: ICX694M (4.5µm x 4.5µm)
TELESCOPE: 132MM APO, 610mm
PRiSMv11, Tycho10.8.4
Site:
ORIGIN: Cepheid Observatory, India
SITELAT: +24:55:00:00
SITELONG:+75:33:58:99
Observers:
Cepheid Observatory
Remark:
Sky Clear

Comet 103P Hartley

cepheids

Image Info:
Object: 103P Hartley
DATE-OBS: 2023 09 20.95559
EXPTIME(mins): 54
SUBFRMS: 27
OBJCTRA: 05 22 56.329
OBJCTDEC: 38 38 18.5
Binning: 1 X 1
Plate Scale: 1.53″ /Pixel
Orientation: North UP/ East Left
Catalogs & Filter Magnitude Results:
Astrometry Catalog: ATLAS
Photometry Catalog: ATLAS
Imaging Filter: CLEAR
Photometry Mag: +13.2 V
Instruments:
CCD: ICX694M (4.5µm x 4.5µm)
TELESCOPE: 132MM APO, 610mm
PRiSMv11, Tycho10.7.5
Site:
ORIGIN: Cepheid Observatory, India
SITELAT: +24:55:00:00
SITELONG:+75:33:58:99
Observers:
Cepheid Observatory
VS Observatory
Remark:
Sky Clear

Photometric Light Curve: SN2023ixf (M101)

cepheids

Object:
SN2023ixf, RA/DEC (2000)
14:03:38.557 +54:18:42.03
Type SN II
Imaging (1): D Singh, India, 0.08m UV/IR+CMOS
Imaging (2): G Visweswaran, USA, 0.33m Lum+CMOS
Imaging (3): Chris Kagy, USA
Measure (1): V K Agnihotri, India
Imaging & Measure (2): Dr. A Raj, 610mm V+CCD, ICSP, Kolkata, India.
Contact mail ID: ashish@csp.res.in , ashishpink@gmail.com
We report V-band photometric observations of SN2023ixf using different size telescopes, namely the 80mm UV/IR+CMOS, India, 330mm Lum + CMOS, USA, 80mm Lum + CMOS,USA and 610mm Vasistha telescope at IERCOO, Sitapur, ICSP, Kolkata. The reported magnitudes also include those obtained from pre-discovery images obtained by D. Singh from Amarkantak, India The supernova was discovered by K. Itagaki on 2023-05-19.727UT. Photometric calibrations are done using Tycho software and ATLAS catalogue.