Four color and H beta photometry of open clusters. IV. h+chi Per.

Crawford, D. L.; Glaspey, J. W.; Perry, C. L.

doi:10.1086/111027

Cited by 60 publications

(69 citation statements)

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“…This procedure follows that described by Crawford, Glaspey, and Perry (1970). The first method utilizes the preliminary calibration of the uvby indices in terms of intrinsic color given by Table I.…”

Section: Discussionmentioning

confidence: 99%

Four-color photometry for the association Lac OB1.

Crawford¹,

Warren²

1976

PASP

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We have obtained uvby data for 51 stars in the region of the association Lacerta OBI, near the 09 V star 10 Lac. An analysis of the present data, combined with previous observations by others, leads to an average color excess for the more concentrated of the two subgroups (lb) of (E(b-y)) = 0 ni 07 ± 0 ni 02 (one star) and an average distance modulus of Vo -M v (ß) = 8 ni 3 ± 0" l 3 (one star). The more dispersed subgroup has a larger average excess and a larger dispersion in both color excess and distance modulus for the stars. Several stars are suggested as nonmembers.

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Section: Discussionmentioning

confidence: 99%

Four-color photometry for the association Lac OB1.

Crawford¹,

Warren²

1976

PASP

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“…Since the original h and s Persei observations (Crawford, Glaspey, & Perry 1970) do not include V values, we used the values given by Johnson & Morgan (1955), which were also taken with the same instrumentation, for the V transformation. The list of standard stars used can be found in Table 2, along with their standard values used for the transformation, taken from and Johnson & Morgan (1955) for h and s Persei, Perry, Lee, & Barnes (1978) for NGC 2169, Crawford, Barnes, & Hill (1977) for NGC 6910, and Canterna, Perry, & Crawford (1979) for NGC 1039.…”

Section: èèèèèèèèèèèèèèèmentioning

confidence: 99%

Photometric and Spectroscopic Study of the Young Open Cluster NGC 1893

Marco

Bernabeu

Negueruela

2001

The Astronomical Journal

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We present uvbyb CCD photometry of the Ðeld of the open cluster NGC 1893. Our photometry is deep enough to cover the complete main-sequence B spectral type. We identify D50 very likely members of the cluster down to spectral type B9ÈA0, some of which have much higher reddenings than the average. We derive a color excess E(b[y) \ 0.33^0.03 and a dereddened distance modulus V 0 [M V \ 13.9^0.2. From the b index, we identify several candidates as emission-line stars, for which we have obtained spectroscopy. Three of them display spectra corresponding to spectral type F but showing Ha in emission. Photometric measurements in this and previous studies indicate strong variability. These characteristics show them to be preÈmain-sequence stars of spectral type F. We also identify two likely Herbig Be stars. These results hint at the existence of a sizable preÈmain-sequence population in NGC 1893.

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“…The double cluster h and Per, the most massive, evolved open cluster within 3 kpc, provides a rich laboratory to study disk evolution in more detail. Starting with the initial study of Oosterhoff (1937), there has been much debate concerning the age, distance, and stellar content of the clusters (e.g., Borgman & Blaauw 1964;Wildey 1964;Schild 1967;Crawford et al 1970;Vogt 1971;Tapia et al 1984;Marco & Bernabeu 2001;Capilla & Fabregat 2002). Recent work (Keller et al 2001;Slesnick et al 2002, hereafter S02;Bragg & Kenyon 2005, hereafter BK05) has converged on a nearly identical age for both clusters, $12Y13 Myr, a common distance of $2.34 kpc (a distance modulus $11.85), a low extinction of E(B À V ) $ 0:5 uniform across the clusters (BK05), and an initial mass function (IMF) of massive stars consistent with results for other young, massive clusters (Massey 2003;Bragg 2004).…”

Section: Introductionmentioning

confidence: 99%

SpitzerIRAC andJHK_sObservations of h and χ Persei: Constraints on Protoplanetary Disk and Massive Cluster Evolution at ∼10⁷Years

Currie¹,

Balog²,

Kenyon³

et al. 2007

ApJ

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We describe IRAC 3.6Y8 m observations and ground-based near-IR JHK s photometry from Mimir and 2MASS of the massive double cluster h and Persei complete to J ¼ 15:5 (M $ 1:3 M ). Within 25 0 of the cluster centers we detect $11,000 sources with J 15:5, $7000 sources with ½4:5 15, and $5000 sources with ½8 14:5. In both clusters the surface density profiles derived from the 2MASS data decline with distance from the cluster centers as expected for a bound cluster. Within 15 0 of the cluster centers, $50% of the stars lie on a reddened $13 Myr isochrone; at 15 0 Y25 0 from the cluster centers, $40% lie on this isochrone. Thus, the optical/2MASS color-magnitude diagrams indicate that h and Per are accompanied by a halo population with roughly the same age and distance as the two dense clusters. The double cluster lacks any clear IR excess sources for J 13:5 ($2.7 M ). Therefore, disks around highmass stars disperse prior to $10 7 yr. At least 2%Y3% of the fainter cluster stars have strong IR excess at both [5.8] and [8]. About 4%Y8% of sources slightly more massive than the Sun ($1.4 M ) have IR excesses at [8]. Combined with the lack of detectable excesses for brighter stars, this result suggests that disks around lower mass stars have longer lifetimes. The IR excess population also appears to be larger at longer IRAC bands ([5.8]

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Four color and H beta photometry of open clusters. IV. h+chi Per.

Cited by 60 publications

References 0 publications

Four-color photometry for the association Lac OB1.

Four-color photometry for the association Lac OB1.

Photometric and Spectroscopic Study of the Young Open Cluster NGC 1893

SpitzerIRAC andJHK_sObservations of h and χ Persei: Constraints on Protoplanetary Disk and Massive Cluster Evolution at ∼10⁷Years

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Four color and H beta photometry of open clusters. IV. h+chi Per.

Cited by 60 publications

References 0 publications

Four-color photometry for the association Lac OB1.

Four-color photometry for the association Lac OB1.

Photometric and Spectroscopic Study of the Young Open Cluster NGC 1893

SpitzerIRAC andJHKsObservations of h and χ Persei: Constraints on Protoplanetary Disk and Massive Cluster Evolution at ∼107Years

Contact Info

Product

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SpitzerIRAC andJHK_sObservations of h and χ Persei: Constraints on Protoplanetary Disk and Massive Cluster Evolution at ∼10⁷Years