UBVRI photometric standard stars in the magnitude range 11.5-16.0 around the celestial equator

Landolt, A. U.

doi:10.1086/116242

Cited by 3,967 publications

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“…These equations are given below: u = U + (6.941 ± 0.007) − (0.011 ± 0.006)(U − B) + (0.516 ± 0.012)X b = B + (4.749 ± 0.007) − (0.044 ± 0.005)(B − V ) + (0.274 ± 0.009)X v = V + (4.313 ± 0.007) − (0.039 ± 0.005)(V − I) + (0.157 ± 0.009)X r = R + (4.222 ± 0.006) − (0.054 ± 0.007)(V − R) + (0.104 ± 0.007)X i = I + (4.711 ± 0.006) − (0.057 ± 0.004)(V − I) + (0.047 ± 0.007)X where U, B, V, R and I are the standard magnitudes, u, b, v, r and i are the instrumental aperture magnitudes normalized for 1 second of exposure time, and X is the airmass. The standard deviations of the differences between the magnitudes calibrated using above transformation equations and the standards given by Landolt (1992) are 0.035, 0.026, 0.025, 0.026 and 0.027 for U, B, V, R and I magnitudes, respectively. The typical Daophot errors in magnitude are found to be large (>0.1 mag) for stars fainter than V ≈21 mag, so the measurements beyond this magnitude are not considered.…”

Section: Optical Datamentioning

confidence: 91%

Stellar contents and star formation in the young cluster Stock 18

2012

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We have carried out deep (V∼21 mag) UBVRI photometric study of the star cluster Stock 18. These along with archival Infrared data have been used to derive the basic cluster parameters and also to study the star formation processes in and around the cluster region. The distance to the cluster is derived as 2.8±0.2 kpc while its age is estimated as 6.0 ± 2.0 Myr. Present study indicates that interstellar reddening is normal in the direction of the cluster. The mass function slope is found to be -1.37±0.27 for the mass range 1< M/M ⊙ <11.9. There is no evidence found for the effect of mass segregation in main-sequence stars of the cluster. A young stellar population with age between 1-2 Myr have been found in and around the cluster region. The presence of IRAS and AKARI sources with MSX intensity map also show the youth of the Sh2-170 region.

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Section: Optical Datamentioning

confidence: 91%

Stellar contents and star formation in the young cluster Stock 18

2012

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“…In all cases, Cousins R filter and aperture photometry were used. Moreover, data from 2004 were absolutely calibrated in the Cousins R system with Landolt (1992) standard stars with absolute errors of 0.01 mag.…”

Section: Optical Disk-integrated Photometrymentioning

confidence: 99%

“…We used standard aperture photometric procedures and performed absolute photometry using at least three Landolt field stars (Landolt 1992). The exposure time was 300 s during all nights, and because of the trailed stars, only absolute photometry was possible.…”

Section: Optical Disk-integrated Photometrymentioning

confidence: 99%

Near-Earth asteroid (3200) Phaethon: Characterization of its orbit, spin state, and thermophysical parameters

Hanuš

Delbò

Vokrouhlický

et al. 2016

A&A

110

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Context. The near-Earth asteroid (3200) Phaethon is an intriguing object: its perihelion is at only 0.14 au and is associated with the Geminid meteor stream. Aims. We aim to use all available disk-integrated optical data to derive a reliable convex shape model of Phaethon. By interpreting the available space-and ground-based thermal infrared data and Spitzer spectra using a thermophysical model, we also aim to further constrain its size, thermal inertia, and visible geometric albedo. Methods. We applied the convex inversion method to the new optical data obtained by six instruments and to previous observations. The convex shape model was then used as input for the thermophysical modeling. We also studied the long-term stability of Phaethon's orbit and spin axis with a numerical orbital and rotation-state integrator.Results. We present a new convex shape model and rotational state of Phaethon: a sidereal rotation period of 3.603958(2) h and ecliptic coordinates of the preferred pole orientation of (319 • , −39 • ) with a 5 • uncertainty. Moreover, we derive its size (D = 5.1 ± 0.2 km), thermal inertia (Γ = 600 ± 200 J m −2 s −1/2 K −1 ), geometric visible albedo (p V = 0.122 ± 0.008), and estimate the macroscopic surface roughness. We also find that the Sun illumination at the perihelion passage during the past several thousand years is not connected to a specific area on the surface, which implies non-preferential heating.

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“…Landolt equatorial standard fields (Landolt 1992) were taken during each of the clear nights so that we could calibrate our frame standards. Saturn was at opposition in January, and so the coverage of Phoebe's light curve in our March data was less complete, although we still managed to obtain two brightness peaks.…”

Section: Observations and Analysismentioning

confidence: 99%

Recovering the Rotational Light Curve of Phoebe

Bauer

Buratti

Simonelli

et al. 2004

ApJ

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We present rotational light-curve data for Saturn's satellite Phoebe taken over the observing period prior to the Cassini mission's encounter with that moon. We find a rotation period of hr, a factor of 9.2735 ‫ע‬ 0.0006 25 improvement in the rotation period's uncertainty over previously published data. This improved rotation period measurement allow s us to correlate previously observed spectral features and colors with albedo features observed by Voyager and to predict which side of Phoebe will be observed by Cassini during its 2004 June 11 encounter. The light curve, sampled at subobserver latitudes farther south than achieved by Voyager, shows evidence of surface features that cannot be explained by previously published shape models or albedo maps and that may be located in the regions in Phoebe's southern hemisphere that were unobserved by Voyager.

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UBVRI photometric standard stars in the magnitude range 11.5-16.0 around the celestial equator

Cited by 3,967 publications

References 0 publications

Stellar contents and star formation in the young cluster Stock 18

Stellar contents and star formation in the young cluster Stock 18

Near-Earth asteroid (3200) Phaethon: Characterization of its orbit, spin state, and thermophysical parameters

Recovering the Rotational Light Curve of Phoebe

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