CCD photometry of late-type stars in the young open cluster IC 2602

Abstract

Abstract. We present the results of V RI photometry of the young open cluster IC 2602. Two 15 arcmin × 15 arcmin fields were observed in February and May 1991 using the 1-m Swope telescope at Las Campanas. Using theoretical isochrones obtained from D' Antona & Mazzitelli (1994), and allowing for observational and other uncertainties, we identify 78 primary candidate members with 12 < V < 18.5 from their positions on colourmagnitude diagrams. We compare the cluster field with an offset field of similar galactic latitude and estimate the contamination due to background stars to be large, ≥ 50%, as might be expected given its low galactic latitude. We also compare our photometry with that given for the X-ray detected stars of Randich et al. (1995). We present complimentary narrow band Hα photometry for a subset of the stars.

Identification of moving groups and member selection usingHipparcosdata*

“…Only recently, using photometric, spectroscopic, and X-ray information, has it become possible to assign membership for fainter stars, V ∼ 10 to ∼18 mag. This resulted in about 50 additional members (see e.g., Prosser, Randich & Stauffer 1996;Stauffer et al 1997;Foster et al 1997;Randich et al 1997). The age estimates range from 8 Myr, based on the ages of the brightest members (Whiteoak 1961;Braes 1962), to 30 Myr, based on isochrone fits to the low mass members .…”

CCD photometry and proper motions of late–type stars in the young open cluster Stock 2

“…This paper is the fourth in a series devoted to finding low mass cluster members in nearby (< 400 pc) open clusters. Previous papers discussed the open clusters NGC 5460 (Barrado & Byrne 1995), IC 2602 (Foster et al 1997) and IC 2391 . As a consequence of the proximity of these open clusters, and the intrinsic faintness of late-type stars, it is difficult to separate cluster members from the field dwarfs and giants.…”

“…Following the same procedure as in Foster et al (1997) and , candidate cluster members were selected using the theoretical pre-main sequence isochrones of D' Antona & Mazzitelli (1994), and in particular those resulting from computations using opacities from Alexander et al (1989) and Rodgers & Iglesias (1992) and the mixing model of Canuto & Mazzitelli (1991).…”

“…In our previous paper, Foster et al (1997) estimated the contamination due to background stars for IC 2602 using CCD observations of an offset field, and as a second approach, by comparison with previously determined star densities for the Pleiades. No offset frame has been observed in the case of Stock 2, and only the latter method can be applied here.…”

Mapping out the Stellar Populations of IC 2602 and IC 2391

“…To study these clusters in detail, a plethora of investigations have been undertaken to identify potential candidate members of IC 2602 and IC 2391 via parallax, proper motion, spatial extent, and photometry (Feinstein 1961;Whiteoak 1961;Braes 1962;Lynga 1962;Foster et al 1997;Rolleston & Byrne 1997;Simon & Patten 1998;Barrado y Navascués et al 2001;Dodd 2004;Randich et al 2005;Gagné et al 2018). Additionally, numerous spectroscopic studies have been conducted to confirm candidate members via signatures of youth (e.g., lithium, Hα, large v i sin ) and stellar properties consistent with those of bona fide cluster members (Buscombe 1965;Abt & Morgan 1972;Levato et al 1988;Messina et al 2003;Paulson & Yelda 2006;Platais et al 2007;Mermilliod et al 2009;De Silva et al 2013;D'Orazi et al 2017;Merle et al 2017).…”