Secondary ${\boldmath UBVRI}$-CCD standard stars   in the 
neighbourhood of Landolt standard stars

Galadí-Enríquez, D.; Trullols, E.; Jordi, C.

doi:10.1051/aas:2000266

Cited by 28 publications

(7 citation statements)

References 8 publications

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“…During the night 28 Feb to 1 March 1998 on La Silla, we also observed several photometric standard stars from Landolt (1992). Also, in the nights 14/15 April 2007 and 23/24 Oct 2008 at GSH, we observed photometric standard stars from Landolt (1992) and Galadi-Enriquez et al (2000) at two or more different airmasses, see Figs. 3 to 5 for those fields and Table 2 for the known magnitudes of the standard stars.…”

Section: Observation and Data Reductionsupporting

confidence: 52%

Photometric monitoring of the young star Par 1724 in Orion

Neuhäuser¹,

Koeltzsch

Raetz

et al. 2009

Astron Nachr

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We report new photometric observations of the ∼ 200 000 year old naked weak-line run-away T Tauri star Par 1724, located north of the Trapezium cluster in Orion. We observed in the broad band filters B, V , R, and I using the 90 cm Dutch telescope on La Silla, the 80 cm Wendelstein telescope, and a 25 cm telescope of the University Observatory Jena in Großschwabhausen near Jena. The photometric data in V and R are consistent with a ∼ 5.7 day rotation period due to spots, as observed before between 1960ies and 2000. Also, for the first time, we present evidence for a long-term 9 or 17.5 year cycle in photometric data (V band) of such a young star, a cycle similar to that to of the Sun and other active stars.

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Section: Observation and Data Reductionsupporting

confidence: 52%

Photometric monitoring of the young star Par 1724 in Orion

Neuhäuser¹,

Koeltzsch

Raetz

et al. 2009

Astron Nachr

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“…Using the Landolt standards, Zhou et al (2001) presented the relationships between the BATC intermediate-band system and U BV RI broadband system by the catalogs of Landolt (1983Landolt ( , 1992 and Galadí-Enríquez et al (2000). We show the coefficients of one relationship in equation (1).…”

Section: Comparison With Previous Photometrymentioning

confidence: 99%

Spectral Energy Distributions and Age Estimates of 78 Star Clusters in M33

Ma¹,

Zhou²,

Chen³

et al. 2002

The Astronomical Journal

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In this third paper of our series, we present CCD spectrophotometry of 78 star clusters that were detected by Chandar, Bianchi, & Ford in the nearby spiral galaxy M33. CCD images of M33 were obtained as a part of the BATC Color Survey of the sky in 13 intermediate-band filters from 3800 to 10000Å. By aperture photometry, we obtain the spectral energy distributions of these 78 star clusters. As Chandar, Bianchi, & Ford did, we estimate the ages of our sample clusters by comparing the photometry of each object with theoretical stellar population synthesis models for different values of metallicity. We find that the sample clusters formed continuously in M33 from ∼ 3 × 10 6 -10 10 years. This conclusion is consistent with Chandar, Bianchi, & Ford. The results also show that, there are two peaks in cluster formation, at ∼ 8 × 10 6 and ∼ 10 9 years in these clusters.

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“…This is caused by the fact that the original photometry in the present paper was obtained in the proprietary BATC filters and transformed to the UBVRI system using transformation equations. Zhou et al (2003) determined these conversions based on the broadband UBVRI magnitudes of 48 stars from Landolt (1983Landolt ( , 1992 and Galadí-Enríquez et al (2000) in the Landolt SA95 field, and their photometric data in the 15 BATC intermediate-band filters. In addition, the central wavelengths and bandwidths of the BATC and UBVRI systems differ.…”

Section: Optical Broadband and Near-infrared 2mass Photometry Of Vdb0mentioning

confidence: 99%

Age and Mass Constraints for a Young Massive Cluster in M31 Based on Spectral Energy Distribution Fitting

Wang

et al. 2011

The Astronomical Journal

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VDB0-B195D is a massive, blue star cluster in M31. It was observed as part of the Beijing-Arizona-TaiwanConnecticut (BATC) Multicolor Sky Survey using 15 intermediate-band filters covering a wavelength range of 3000-10000 Å. Based on aperture photometry, we obtain its spectral energy distribution (SED) as defined by the 15 BATC filters. We apply previously established relations between the BATC intermediate-band and the Johnson-Cousins UBVRI broadband systems to convert our BATC photometry to the standard system. A detailed comparison shows that our newly derived VRI magnitudes are fully consistent with previous results, while our new B magnitude agrees to within 2σ . In addition, we determine the cluster's age and mass by comparing its SED (from 3000 to 20000 Å, comprising photometric data in the 15 BATC intermediate bands, optical broadband BVRI, and Two Micron All Sky Survey near-infrared JHK s data) with theoretical stellar population synthesis models, resulting in age and mass determinations of 60.0±8.0 Myr and (1.1-1.6)×105 M , respectively. This age and mass confirms previous suggestions that VDB0-B195D is a young massive cluster in M31.

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Secondary ${\boldmath UBVRI}$-CCD standard stars in the neighbourhood of Landolt standard stars

Cited by 28 publications

References 8 publications

Photometric monitoring of the young star Par 1724 in Orion

Photometric monitoring of the young star Par 1724 in Orion

Spectral Energy Distributions and Age Estimates of 78 Star Clusters in M33

Age and Mass Constraints for a Young Massive Cluster in M31 Based on Spectral Energy Distribution Fitting

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