J/AJ/148/85 WIYN open cluster study. LXII. Photometry of M35 (Thompson+, 2014)
WIYN open cluster study. LXII. Comparison of isochrone systems using deep
multi-band photometry of M35.
Thompson B., Frinchaboy P., Kinemuchi K., Sarajedini A., Cohen R.
<Astron. J., 148, 85 (2014)>
=2014AJ....148...85T 2014AJ....148...85T
ADC_Keywords: Clusters, open ; Photometry, UBVRI ; Photometry, infrared
Keywords: open clusters and associations: general -
open clusters and associations: individual: M35
Abstract:
The current generation of stellar isochrone models exhibits
non-negligible discrepancies due to variations in the input physics.
The success of each model is determined by how well it fits the
observations, and this paper aims to disentangle contributions from
the various physical inputs. New deep, wide-field optical and
near-infrared photometry (UBVRIJHKS) of the cluster M35 is
presented, against which several isochrone systems are compared:
Padova, PARSEC, Dartmouth, and Y2. Two different atmosphere models
are applied to each isochrone: ATLAS9 and BT-Settl. For any isochrone
set and atmosphere model, observed data are accurately reproduced for
all stars more massive than 0.7M☉. For stars less massive than
0.7M☉, Padova and PARSEC isochrones consistently produce higher
temperatures than observed. Dartmouth and Y2 isochrones with
BT-Settl atmospheres reproduce optical data accurately; however, they
appear too blue in IR colors. It is speculated that molecular
contributions to stellar spectra in the near-infrared may not be fully
explored, and that future study may reconcile these differences.
Description:
Using the Kitt Peak National Observatory (KPNO) 0.9m MOSAIC camera, a
59'*59' field of view has been observed in UBVRI. M35 images, observed
over two nights in 2000 February, were taken in two sequences: short
and long, allowing for the photometry of both the brightest and
faintest stars in the cluster.
JHKs observations of M35 were taken using the NEWFIRM instrument on
the Kitt Peak 4m Telescope in 2008 February. The NEWFIRM camera is a
grid of four 2k*2k IR detectors, creating a 4k*4k image.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 121 39757 Combined data set photometry of M35
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See also:
B/ocl : Optically visible open clusters and Candidates (Dias+ 2002-2014)
J/A+A/564/A42 : Δa-photometry in 10 open clusters (Paunzen+, 2014)
J/AJ/139/1383 : Radial velocities in M35 (NGC 2168) (Geller+, 2010)
J/ApJ/695/679 : Stellar rotation in M35 (Meibom+, 2009)
J/AJ/133/394 : Low-mass binary companions in M35 (McNamara+, 2007)
J/ApJ/546/1006 : VRI photometry of M35 (Barrado y Navascues+, 2001)
J/MNRAS/306/361 : UBVI CCD photometry of M35 (NGC 2168) (Sung+ 1999)
Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 F8.5 deg RAdeg Right Ascension in decimal degrees (J2000)
10- 17 F8.5 deg DEdeg Declination in decimal degrees (J2000)
19- 24 F6.3 mag Umag [9.6/19.8]?=99.999 The KPNO U magnitude
26- 30 F5.3 mag e_Umag ?=9.999 Uncertainty in Umag
32- 37 F6.3 mag Bmag [9.8/20.8]?=99.999 The KPNO B magnitude
39- 43 F5.3 mag e_Bmag ?=9.999 Uncertainty in Bmag
45- 50 F6.3 mag Vmag [9.8/19.8]?=99.999 The KPNO V magnitude
52- 56 F5.3 mag e_Vmag ?=9.999 Uncertainty in Vmag
58- 63 F6.3 mag Rmag [9.7/19.2]?=99.999 The KPNO R magnitude
65- 69 F5.3 mag e_Rmag ?=9.999 Uncertainty in Rmag
71- 76 F6.3 mag Imag [9.5/18.5]?=99.999 The KPNO I magnitude
78- 82 F5.3 mag e_Imag ?=9.999 Uncertainty in Imag
84- 89 F6.3 mag Jmag [13.1/19.1]?=99.999 The NEWFIRM J magnitude
91- 95 F5.3 mag e_Jmag ?=9.999 Uncertainty in Jmag (1)
97-102 F6.3 mag Hmag [12.0/18.9]?=99.999 The NEWFIRM H magnitude
104-108 F5.3 mag e_Hmag ?=9.999 Uncertainty in Hmag (1)
110-115 F6.3 mag Ksmag [12.0/18.2]?=99.999 The NEWFIRM Ks (short)
magnitude (1)
117-121 F5.3 mag e_Ksmag ?=9.999 Uncertainty in Ksmag
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Note (1): 2MASS data were used to tie the instrumental NEWFIRM magnitudes to
the standard system. See section 2.2 for further details.
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History:
From electronic version of the journal
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(End) Greg Schwarz [AAS], Sylvain Guehenneux [CDS] 05-Dec-2014