Atmospheric Intensity Scintillation of Stars. III. Effects for Different Telescope Apertures: Erratum

Dravins, Dainis; Lindegren, L.; Mezey, E.; Young, A. T.

doi:10.1086/316232

Cited by 11 publications

(7 citation statements)

References 0 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…As far as scintillation noise is concerned on the one hand, its level can be reduced by increasing the size of the telescope and by observing at a lower airmass (Young 1967;Dravins et al 1998). These two factors will be improved in the future since ARIES is building a 1.3-m telescope 50 km further away in the mountains, and at a higher altitude (Devasthal site, 2420 m instead of 1951 m at Manora Peak).…”

Section: Null Resultsmentioning

confidence: 99%

The Nainital-Cape Survey

Joshi¹,

Mary²,

Martinez³

et al. 2006

A&A

View full text Add to dashboard Cite

Aims. We search for photometric variability in chemically peculiar A type stars in the northern hemisphere. Methods. High-speed photometric observations of Ap and Am star candidates have been carried out from ARIES (Manora Peak, Nainital) using a three-channel fast photometer attached to the ARIES 104-cm Sampurnanand telescope.Results. This paper presents three new variables: HD 113878, HD 118660 and HD 207561. During the time span of the survey (1999 December to 2004 January) pulsations of the δ Sct type were also found for the two evolved Am stars HD 102480 and HD 98851, as reported in Joshi et al. (2002Joshi et al. ( , 2003. Additionally, we present 140 null results of the survey for this time span. Conclusions. The star HD 113878 pulsates with a period of 2.31 h, which is typical of δ Sct stars. HD 118660 exhibits multi-periodic variability with a prominent period of nearly 1 h. These periods need to be investigated and make HD 118660 a particularly interesting target for further observations. For HD 207561, a star classified as Am, a probable pulsation with a period of 6 min was found in the light curves obtained on two consecutive nights. Both HD 102480 and HD 98851 exhibit unusual alternating high and low amplitude maxima, with a period ratio of 2:1. The analysis of the null results confirms the photometric quality of the Nainital site.

show abstract

Section: Null Resultsmentioning

confidence: 99%

The Nainital-Cape Survey

Joshi¹,

Mary²,

Martinez³

et al. 2006

A&A

View full text Add to dashboard Cite

show abstract

“…The standard deviation of all 30 measurements of the target star is 7.7 mmag. The scatter within each triplet of observations made in quick succession increases with air mass A approximately as expected for scintillation, 2:8 1:75 mmag rms per measurement (Dravins et al 1998;eq.[10]). Shot noise contributes 1.4 mmag rms per measurement.…”

Section: Photometric Observations Of Hd 109749 With the Smarts Telescmentioning

confidence: 72%

The N2K Consortium. III. Short‐Period Planets Orbiting HD 149143 and HD 109749

Fischer

Laughlin

Marcy

et al. 2006

ApJ

View full text Add to dashboard Cite

We report the detection of two short-period planets discovered at Keck Observatory. HD 149143 is a metal-rich G0 IV star with a planet of M sin i ¼ 1:33M J and an orbital radius of 0.053 AU. The best-fit Keplerian model has an orbital period, P ¼ 4:072 days, semivelocity amplitude, K ¼ 149:6 m s À1 , and eccentricity, e ¼ 0:016 AE 0:01. The host star is chromospherically inactive and metal-rich, with ½Fe/ H ¼ 0:26. Based on the T eA and stellar luminosity, we derive a stellar radius of 1.49 R . Photometric observations of HD 149143 were carried out using the automated photometric telescopes at Fairborn Observatory. HD 149143 is photometrically constant over the radial velocity period to 0:0003 AE 0:0002 mag, supporting the existence of the planetary companion. No transits were detected down to a photometric limit of approximately 0.02%, eliminating transiting planets with a variety of compositions and constraining the orbital inclination to less than 83 . A short-period planet was also detected around HD 109749, a G3 IV star. HD 109749 is chromospherically inactive, with ½Fe/H ¼ 0:25 and a stellar radius of 1.24. The radial velocities for HD 109749 are modeled by a Keplerian with P ¼ 5:24 days and K ¼ 28:7 m s À1 . The inferred planet mass is M sin i ¼ 0:28M J and the semimajor axis of this orbit is 0.0635 AU. Photometry of HD 109749 was obtained with the SMARTS consortium telescope, the PROMPT telescope, and by transitsearch.org observers in Adelaide and Pretoria. These observations did not detect a decrement in the brightness of the host star at the predicted ephemeris time, and they constrain the orbital inclination to less than 85 for gas giant planets with radii down to 0:7R J .

show abstract

“…We calculate scintillation noise using the method described by Young (1967) and by Dravins et al (1998), which is given by…”

Section: Muscat and Muscat2 Simulation Toolsmentioning

confidence: 99%

Simulations Predicting the Ability of Multi-color Simultaneous Photometry to Distinguish TESS Candidate Exoplanets from False Positives

Louie

Narita

Fukui

et al. 2020

PASP

View full text Add to dashboard Cite

The Transiting Exoplanet Survey Satellite (TESS) is currently concluding its 2-year primary science mission searching 85% of the sky for transiting exoplanets. TESS has already discovered well over one thousand TESS objects of interest (TOIs), but these candidate exoplanets must be distinguished from astrophysical false positives using other instruments or techniques. The 3-band Multi-color Simultaneous Camera for Studying Atmospheres of Transiting Planets (MuSCAT), as well as the 4-band MuSCAT2, can be used to validate TESS discoveries. Transits of exoplanets are achromatic when observed in multiple bandpasses, while transit depths for false positives often vary with wavelength. We created software tools to simulate MuSCAT/MuSCAT2 TESS follow-up observations and reveal which planet candidates can be efficiently distinguished from blended eclipsing binary (BEB) false positives using these two instruments, and which must be validated using other techniques. We applied our software code to the Barclay et al. (2018) predicted TESS discoveries, as well as to TOIs downloaded from the ExoFOP-TESS website. We estimate that MuSCAT (MuSCAT2 values in parentheses) will be able to use its multi-color capabilities to distinguish BEB false positives for ∼17% (∼18%) of all TESS discoveries, and ∼13% (∼15%) of R pl < 4R ⊕ discoveries. Our TOI analysis shows that MuSCAT (MuSCAT2) can distinguish BEB false positives for ∼55% (∼52%) of TOIs with transit depths greater than 0.001, for ∼64% (∼61%) of TOIs with transit depths greater than 0.002, and for ∼70% (∼68%) of TOIs with transit depth greater than 0.003. Our work shows that MuSCAT and MuSCAT2 can validate hundreds of R pl < 4R ⊕ candidate exoplanets, thus supporting the TESS mission in achieving its Level 1 Science Requirement of measuring the masses of 50 exoplanets smaller in size than Neptune. Our software tools will assist scientists as they prioritize and optimize follow-up observations of TESS objects of interest.

show abstract

Atmospheric Intensity Scintillation of Stars. III. Effects for Different Telescope Apertures: Erratum

Cited by 11 publications

References 0 publications

The Nainital-Cape Survey

The Nainital-Cape Survey

The N2K Consortium. III. Short‐Period Planets Orbiting HD 149143 and HD 109749

Simulations Predicting the Ability of Multi-color Simultaneous Photometry to Distinguish TESS Candidate Exoplanets from False Positives

Contact Info

Product

Resources

About