The USNO-B Catalog

Monet, D. G.; Levine, S. E.; Canzian, B.; Ables, H. D.; Bird, A. J.; Dahn, C. C.; Guetter, H. H.; Harris, Hugh C.; Henden, A. A.; Leggett, S. K.; Levison, H. F.; Luginbuhl, C. B.; Martini, Juliane; Monet, A. B.; Munn, Jeffrey A.; Pier, Jeffrey R.; Rhodes, A.; Riepe, B. Y.; Sell, Saskia; Stone, R. C.; Vrba, F. J.; Walker, Richard L.; Westerhout, G.; Brucato, R. J.; Reid, Neill; Schoening, W. E.; Hartley, Matthew; Read, Mike; Tritton, S. B.

doi:10.1086/345888

Cited by 2,124 publications

(2,006 citation statements)

References 13 publications

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“…4). HH 892A has the entry 1443−0136438 in the USNO-B1.0 catalogue (Monet et al 2003) with R POSS−I = 19.59 mag, R POSS−II = 19.20 mag, and zero proper motion. The CCD R magnitude amounts to 19.65 ± 0.43 mag.…”

Section: The Herbig-haro Flowmentioning

confidence: 99%

The new nebula in LDN 1415 – A cry from the cradle of a low-luminosity source

Stecklum¹,

Melnikov

Meusinger³

2006

A&A

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Aims.A survey for candidate Herbig-Haro objects was performed to search for evidence of star formation in Galactic dark clouds Methods. For this aim true colour images were created from blue, red, and infrared DSS2 plates and inspected. Follow-up I-band, Hα, and [S ii] CCD imaging as well as long-slit spectroscopy using the Tautenburg 2-m telescope was carried out to verify candidate objects.Results. In the case of LDN 1415, the presence of a Herbig-Haro flow could be revealed which is henceforth named HH 892. In addition, an arcuate nebula was found which is barely seen on the DSS2 infrared plate (epoch 1996) and not detected in archival Kiso Schmidt data (epoch 2001). Thus, this nebula must have brightened by about 3.8 mag in recent years. Conclusions. The nebula is associated with IRAS 04376+5413. The 2MASS images show a red counterpart of the IRAS source, designated as L1415-IRS. Its morphology resembles that of a bipolar young object. The luminosity of this source integrated from 0.9 µm to 60 µm in the low state amounts to 0.13 L for an assumed distance of 170 pc. Thus it seems to be a young very-low mass star or it might even be of substellar mass. The current brightness increase of the nebula is caused by a FUor-or EXor-like outburst as indicated by the presence of a P Cygni profile of the Hα line. L1415-IRS is by far the least luminous member of the sparse sample of FUor and EXor objects.

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Section: The Herbig-haro Flowmentioning

confidence: 99%

The new nebula in LDN 1415 – A cry from the cradle of a low-luminosity source

Stecklum¹,

Melnikov

Meusinger³

2006

A&A

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“…However, the cutoff of the GSC-I at relatively bright magnitudes (m ≤ 15) admittedly represents a significant limit for it being used as a reference for the compilation of a new PN catalogue. Similarly, the USNO-A2.0 (Monet et al 1998) did not provide all the information necessary for our project. We therefore took up the task of providing to the community a dedicated PN catalogue taking advantage of the recently released Guide Star Catalogue II 1 (McLean et al 2000), making its gains in accuracy and homogeneity readily available.…”

Section: The Choice Of the Reference Cataloguementioning

confidence: 99%

Galactic Planetary Nebulae and their central stars

Kerber¹,

Mignani²,

Guglielmetti

et al. 2003

A&A

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Abstract. We have used the 2nd generation of the Guide Star Catalogue (GSC-II) as a reference astrometric catalogue to compile the positions of 1086 Galactic Planetary Nebulae (PNe) listed in the Strasbourg ESO Catalogue (SEC), its supplement and the version 2000 of the Catalogue of Planetary Nebulae. This constitutes about 75% of all known PNe. For these PNe, the ones with a known central star (CS) or with a small diameter, we have derived coordinates with an absolute accuracy of ≈0. 35 in each coordinate, which is the intrinsic astrometric precision of the GSC-II. For another 226, mostly extended, objects without a GSC-II counterpart we give coordinates based on the second epoch Digital Sky Survey (DSS-II). While these coordinates may have systematic offsets relative to the GSC-II of up to 5 arcsecs, our new coordinates usually represent a significant improvement over the previous catalogue values for these large objects. This is the first truly homogeneous compilation of PNe positions over the whole sky and the most accurate one available so far.

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“…For the purposes outlined in the previous section, we will make use of the USNO-B1 catalog (Monet et al 2003) which provides astrometric positions and their uncertainties, and photographic photometry on various optical bands for a complete set of stars brighter than V ∼ 21 with an overall 0.2 arcsec astrometric accuracy at J2000 and ∼0.3 mag photometric accuracy. In addition, for each entry the catalog provides a star/galaxy index, which is believed to be 85% accurate at distinguishing stars from non-stellar sources.…”

Section: Prior Information and Incremental Observationsmentioning

confidence: 99%

Analysis of the Bayesian Cramér-Rao lower bound in astrometry

Echeverria

Silva

Mendez

et al. 2016

A&A

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Context. The best precision that can be achieved to estimate the location of a stellar-like object is a topic of permanent interest in the astrometric community. Aims. We analyze bounds for the best position estimation of a stellar-like object on a CCD detector array in a Bayesian setting where the position is unknown, but where we have access to a prior distribution. In contrast to a parametric setting where we estimate a parameter from observations, the Bayesian approach estimates a random object (i.e., the position is a random variable) from observations that are statistically dependent on the position. Methods. We characterize the Bayesian Cramér-Rao (CR) that bounds the minimum mean square error (MMSE) of the best estimator of the position of a point source on a linear CCD-like detector, as a function of the properties of detector, the source, and the background.Results. We quantify and analyze the increase in astrometric performance from the use of a prior distribution of the object position, which is not available in the classical parametric setting. This gain is shown to be significant for various observational regimes, in particular in the case of faint objects or when the observations are taken under poor conditions. Furthermore, we present numerical evidence that the MMSE estimator of this problem tightly achieves the Bayesian CR bound. This is a remarkable result, demonstrating that all the performance gains presented in our analysis can be achieved with the MMSE estimator. Conclusions. The Bayesian CR bound can be used as a benchmark indicator of the expected maximum positional precision of a set of astrometric measurements in which prior information can be incorporated. This bound can be achieved through the conditional mean estimator, in contrast to the parametric case where no unbiased estimator precisely reaches the CR bound.

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The USNO-B Catalog

Cited by 2,124 publications

References 13 publications

The new nebula in LDN 1415 – A cry from the cradle of a low-luminosity source

The new nebula in LDN 1415 – A cry from the cradle of a low-luminosity source

Galactic Planetary Nebulae and their central stars

Analysis of the Bayesian Cramér-Rao lower bound in astrometry

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