Exo-Planet, Class confirmed: TOI-3819b (High) 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 = 0.0885 ± 0.0071 (expected: 0.07829431652425353 ± 0.000830200746178871) O-C = -3.21 ± 6.62 minutes Diagnostics Transit SNR = 6.27 (good:≥5, acceptable:≥3) (strong detection of the transit) Rp/Rs drift = 1.43σ (good:≤2, acceptable:≤3) (Rp/Rs in good agreement with the literature) AutoCorrelation = 0.205 (good:≤0.353, acceptable:≤0.433) (no systematics in the data) Shapiro = 0.004 (good:≤0.042, acceptable:≤0.07) (few or no outliers in the data)
Exo-Planet, Class confirmed: WASP-11b 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 Haze
Results Rp/Rs = 0.1297 ± 0.0035 (expected: 0.131 ± 0.0008) O-C = 0.87 ± 1.32 minutes Quality check Residuals STD (Standard Deviation) = 3.612 ‰ Diagnostics Step 1: Transit SNR = 18.58 Transit SNR is good (strong detection of the transit) Step 2: Rp/Rs drift = -0.36σ The Rp/Rs drift is good (Rp/Rs in good agreement with the literature) Step 3: Auto Correlation = 0.379 Step 4: Shapiro test = 0.015 The Shapiro test is good (few or no outliers in the data)
Exo-Planet, Class confirmed: WASP-32b 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 = 0.1062 ± 0.0027 (expected: 0.1114 ± 0.0018) O-C = -0.89 ± 1.58 minutes Diagnostics Transit SNR = 19.74 (good:≥5, acceptable:≥3) (strong detection of the transit) Rp/Rs drift = -1.6σ (good:≤2, acceptable:≤3) (Rp/Rs in good agreement with the literature) AutoCorrelation = 0.268 (good:≤0.355, acceptable:≤0.436) (no systematics in the data) Shapiro = 0.016 (good:≤0.042, acceptable:≤0.071) (few or no outliers in the data)
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)
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)
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)
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)
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)!
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
