Photometry of the α Persei Cluster.

Mitchell, R. I.

doi:10.1086/146902

Cited by 32 publications

(26 citation statements)

References 0 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…A CCD UBV(RI) C survey of northern OCs has been undertaken at SPMO using always the same instrumental setup (telescope, CCD, filters), observing and data reduction procedures, and system of standard stars (Landolt , 1983(Landolt , , 1992Clem & Landoldt , 2013;Michel , 2014). The CCD UBV(RI) C observations of the 20 OCs of this paper have been made exclusively with the 0.84-m f/13 Cassegrain telescope of SPMO, during nights of June 2001, February 2002 (subdiveded in four contigous nights to check the night parameters) and January, May (subdiveded as February 2002 for the same reason), September, and November 2003.…”

Section: Observations and Reduction Proceduresmentioning

confidence: 99%

“…Several standard-star fields from Landolt (1992) ;Clem & Landoldt (2013);Michel (2014) were observed to permit the determination of the atmospheric extinction coefficients and the derivation of the photometric transformations to the Johnson-Cousins photometric system 3 . The standard-star fields have been observed with exposures of 1 × 240 seconds for the U filter, 1 × 120 for B, 1 × 60 for V, 1 × 60 for R and I.…”

Section: Observations and Reduction Proceduresmentioning

confidence: 99%

“…Standard, absolute photometry outside the earth's atmosphere has usually been reduced from a instrumental to a standard or reference system with two forms of equations: one deducing stellar colours in a standard or reference system, based on a subset of the reference stars measured with the same instrumental set-up one is calibrating, and the other one deducing magnitudes in the standard system (Mitchell , 1960;Hardie , 1962, c.f.). The following is an equality relating instrumental colours with their equivalent standard values:…”

Section: Observations and Reduction Proceduresmentioning

confidence: 99%

See 2 more Smart Citations

CCD UBV(RI)C photometry of twenty open clusters

Oralhan¹,

Karataş²,

Schuster³

et al. 2015

New Astronomy

View full text Add to dashboard Cite

Fundamental astrophysical parameters have been derived for 20 open clusters (OCs) using CCD UBV(RI) C photometric data observed with the 84 cm telescope at the San Pedro Mártir National Astronomical Observatory, México.The interstellar reddenings, metallicities, distances, and ages have been compared to the literature values. Significant differences are usually due to the usage of diverse empirical calibrations and differing assumptions, such as concerning cluster metallicity, as well as distinct isochrones which correspond to differing element-abundance ratios, internal stellar physics, and photometric systems. Different interstellar reddenings, as well as varying reduction and cluster-membership techniques, are also responsible for these kinds of systematic differences and errors.The morphological ages, which are derived from the morphological indices (δV and δ1) in the CM diagrams, are in good agreement with the isochrone ages of 12 OCs, those with good red clump (RC) and red giant (RG) star candidates. No metal abundance gradient is detected for the range 6.82 ≤ R GC ≤ 15.37 kpc, nor any correlation between the cluster ages and metal abundances for these 20 OCs.Young, metal-poor OCs, observed here in the third Galactic quadrant, may be associated with stellar over-densities, such as that in Canis Major (Martin et al.) and the Monoceros Ring (Newberg et al.), or signatures of past accretion events, as discussed by Yong et al. and Carraro et al.

show abstract

Section: Observations and Reduction Proceduresmentioning

confidence: 99%

Section: Observations and Reduction Proceduresmentioning

confidence: 99%

Section: Observations and Reduction Proceduresmentioning

confidence: 99%

See 1 more Smart Citation

CCD UBV(RI)C photometry of twenty open clusters

Oralhan¹,

Karataş²,

Schuster³

et al. 2015

New Astronomy

View full text Add to dashboard Cite

show abstract

“…Mitchell 1960;Fresneau 1980;Prosser 1992Prosser , 1994, the IMF of this object has not been investigated since the work of Tarrab (1982).…”

Section: α Per (Melotte 20)mentioning

confidence: 99%

The IMF of open star clusters with Tycho-2

Sanner

Geffert

2001

A&A

View full text Add to dashboard Cite

Abstract. We studied the fields of nine nearby open star clusters based on the Tycho-2 catalogue. We determined membership probabilities for the stars in the cluster fields from the stellar proper motions and used the Tycho-2 photometry to compute the initial mass function (IMF) of the clusters from the main sequence turn-off point down to approx. 1 M . We found IMF slopes ranging from Γ = −0.69 down to Γ = −2.27 (when the Salpeter 1955 value would be Γ = −1.35). We also studied the membership of individual stars of special astrophysical interest. In some cases previous results had to be revised. As a by-product, we investigated some general properties of the Tycho-2 catalogue; we confirmed that the Tycho-2 proper motions show only marginal deviations from the Hipparcos catalogue. On the other hand, in some regions the completeness of the catalogue seems to decrease at magnitudes brighter than claimed by Høg et al. (2000).

show abstract

“…The data at each night were reduced independently following a standard procedure (e.g. Mitchell 1960). The resulting photometry of the program stars is given in Table 5.…”

Section: Jhkl Photometrymentioning

confidence: 99%

New weak-line T Tauri stars in Orion from the ROSAT all-sky survey

Alcalá

Terranegra

Wichmann³

et al. 1996

Astron. Astrophys. Suppl. Ser.

View full text Add to dashboard Cite

Abstract. -We present results of the spectroscopic and photometric follow-up observations of the ROSAT allsky survey in the direction of the Orion cloud complex. The main goal of these observations is the search for X-ray emitting pre-main sequence stars. 820 X-ray sources were detected with high confidence in about 450 square degrees. The mean density of X-ray sources in this region is a factor of about two higher than that of the whole RASS. 5% of the RASS sources in this region are identified with previously known and likely pre-main sequence stars. We have investigated spectroscopically 181 new RASS sources widely distributed over the entire cloud complex. On the basis of the presence of strong Li I λ6707 absorption, spectral type later than F0 and chromospheric emission, 112 new weak-line T Tauri stars could be found. We present coordinates, X-ray count-rates and finding charts of the new PMS. Optical UBV (RI)KC, near-infrared JHKLM and uvby-β photometry for the new WTTS is also provided. In addition 24 dKe-dMe stars were also found on the basis of the RASS data.

show abstract

Photometry of the α Persei Cluster.

Cited by 32 publications

References 0 publications

CCD UBV(RI)C photometry of twenty open clusters

CCD UBV(RI)C photometry of twenty open clusters

The IMF of open star clusters with Tycho-2

New weak-line T Tauri stars in Orion from the ROSAT all-sky survey

Contact Info

Product

Resources

About