383 research outputs found
Astrometric proof of companionship for the L dwarf companion candidate GJ 1048B
Gizis et al. (2001) reported a companion candidate of spectral type L1 near
the K2 dwarf GJ 1048 using the Two Micron All-Sky Survey (2MASS). At that time
it was not possible to verify companionship astrometrically using the 2MASS
data alone due to the small proper motion of GJ 1048. We now show that both
objects share the same proper motion by using data from the UK Schmidt
Telescope Near-infrared (IVN) Southern Survey as the first epoch and data from
2MASS as the second epoch. Our technique of subtracting the PSF of the primary
from the SuperCOSMOS I scans of the Southern Survey enables the astrometry of
the companion candidate to be measured directly.Comment: Accepted to A&A 2004/03/14, 3 pages, 4 figure
Revised metallicity classes for low-mass stars: dwarfs (dM), subdwarfs (sdM), extreme subdwarfs (esdM), and ultra subdwarfs (usdM)
The current classification system of M stars on the main sequence
distinguishes three metallicity classes (dwarfs - dM, subdwarfs - sdM, and
extreme subdwarfs - esdM). The spectroscopic definition of these classes is
based on the relative strength of prominent CaH and TiO molecular absorption
bands near 7000A, as quantified by three spectroscopic indices (CaH2, CaH3, and
TiO5). We re-examine this classification system in light of our ongoing
spectroscopic survey of stars with proper motion \mu > 0.45 "/yr, which has
increased the census of spectroscopically identified metal-poor M stars to over
400 objects. Kinematic separation of disk dwarfs and halo subdwarfs suggest
deficiencies in the current classification system. Observations of common
proper motion doubles indicates that the current dM/sdM and sdM/esdM boundaries
in the [TiO5,CaH2+CaH3] index plane do not follow iso-metallicity contours,
leaving some binaries inappropriately classified as dM+sdM or sdM+esdM. We
propose a revision of the classification system based on an empirical
calibration of the TiO/CaH ratio for stars of near solar metallicity. We
introduce the parameter \zeta_{TiO/CaH} which quantifies the weakening of the
TiO bandstrength due to metallicity effect, with values ranging from
\zeta_{TiO/CaH}=1 for stars of near-solar metallicity to \zeta_{TiO/CaH}~0 for
the most metal-poor (and TiO depleted) subdwarfs. We redefine the metallicity
classes based on the value of the parameter \zeta_{TiO/CaH}; and refine the
scheme by introducing an additional class of ultra subdwarfs (usdM). We
introduce sequences of sdM, esdM, and usdM stars to be used as formal
classification standards.Comment: 15 pages, accepted for publication in the Astrophysical Journa
A Chandra X-ray detection of the L dwarf binary Kelu-1: Simultaneous Chandra and Very Large Array observations
Magnetic activity in ultracool dwarfs, as measured in X-rays and H,
shows a steep decline after spectral type M7-M8. So far, no L dwarf has been
detected in X-rays. In contrast, L dwarfs may have higher radio activity than M
dwarfs. We observe L and T dwarfs simultaneously in X-rays and radio to
determine their level of magnetic activity in the context of the general
decline of magnetic activity with cooler effective temperatures. The field L
dwarf binary Kelu-1 was observed simultaneously with Chandra and the Very Large
Array. Kelu-1AB was detected in X-rays with erg/s, while it remained undetected in the radio down to a limit of erg/s/Hz. We argue that,
whereas the X-ray and H emissions decline in ultracool dwarfs with
decreasing effective temperature, the radio luminosity stays (more or less)
constant across M and early-L dwarfs. The radio surface flux or the luminosity
may better trace magnetic activity in ultracool dwarfs than the ratio of the
luminosity to the bolometric luminosity. Deeper radio observations (and at
short frequencies) are required to determine if and when the cut-off in radio
activity occurs in L and T dwarfs, and what kind of emission mechanism takes
place in ultracool dwarfs.Comment: Accepted for publication as a Letter in Astronomy & Astrophysic
The Trigonometric Parallax of the Brown Dwarf Planetary System 2MASSW J1207334-393254
We have measured a trigonometric parallax to the young brown dwarf 2MASSW
J1207334-393254. The distance [54.0 (+3.2,-2.8) pc] and space motion confirm
membership in the TW Hydrae Association. The primary is a ~25 M_jup brown
dwarf. We discuss the "planetary mass" secondary, which is certainly below the
deuterium-burning limit but whose colors and absolute magnitudes pose
challenges to our current understanding of planetary-mass objects.Comment: Accepted to the Astrophysical Journal Letter
Giant Planet Companion to 2MASSW J1207334-393254
We report new VLT/NACO imaging observations of the young, nearby brown dwarf
2MASSW J1207334-393254 and its suggested planetary mass companion (2M1207 b).
Three epochs of VLT/NACO measurements obtained over nearly one year show that
the planetary mass companion candidate shares the same proper motion and, with
a high confidence level, is not a stationary background object. This result
confirms the status of 2M1207 b as of planetary mass (5 times the mass of
Jupiter) and the first image of a planetary mass companion in a different
system than our own. This discovery offers new perspectives for our
understanding of chemical and physical properties of planetary mass objects as
well as their mechanisms of formation.Comment: 4 pages, 2 figures. accepted in Astronomy & Astrophysic
A Deep Look at the T-Type Brown Dwarf Binary Indi Bab with Chandra and ATCA
We present deep observations of the nearby T-type brown dwarf binary
Indi Bab in radio with the Australia Telescope Compact Array and in
X-rays with the Chandra X-ray Observatory. Despite long integration times, the
binary (composed of T1 and T6 dwarfs) was not detected in either wavelength
regime. We reached upper limits of and erg/s/Hz for the radio luminosity at 4.8 GHz and 8.64 GHz,
respectively; in the X-rays, the upper limit in the keV band was erg/s. We discuss the above results in the framework of
magnetic activity in ultracool, low-mass dwarfs.Comment: Accepted for publication in the Astrophysical Journal Letter
A Global Photometric Analysis of 2MASS Calibration Data
We present results from the application of a global photometric calibration
(GPC) procedure to calibration data from the first 2 years of The Two Micron
All Sky Survey (2MASS). The GPC algorithm uses photometry of both primary
standards and moderately bright `tracer' stars in 35 2MASS calibration fields.
During the first two years of the Survey, each standard was observed on
approximately 50 nights, with about 900 individual measurements. Based on the
photometry of primary standard stars and secondary tracer stars and under the
assumption that the nightly zeropoint drift is linear, GPC ties together all
calibration fields and all survey nights simultaneously, producing a globally
optimized solution. Calibration solutions for the Northern and Southern
hemisphere observatories are found separately, and are tested for global
consistency based on common fields near the celestial equator.
Several results from the GPC are presented, including establishing candidate
secondary standards, monitoring of near-infrared atmospheric extinction
coefficients, and verification of global validity of the standards. The
solution gives long-term averages of the atmospheric extinction coefficients,
A_J=0.096, A_H=0.026, A_{K_s}=0.066 (North) and A_J=0.092, A_H=0.031,
A_{K_s}=0.065 (South), with formal error of 0.001. The residuals show small
seasonal variations, most likely due to changing atmospheric content of water
vapor. Extension of the GPC to approximately 100 field stars in each of the 35
calibration fields yields a catalog of more than two thousand photometric
standards ranging from 10th to 14th magnitude, with photometry that is globally
consistent to .Comment: 19 pages, 10 figures; Submitted to AJ. The table of secondary
standards is available from ftp://nova.astro.umass.edu/pub/nikolaev/ or
ftp://anon-ftp.ipac.caltech.edu/pub/2mass/globalcal
Faint M-dwarfs and the structure of the Galactic disk
We use broadband photometry and low-resolution spectra of a complete sample
of late-K and M dwarfs brighter than I=22 in three fields at high galactic
latitude to study issues relating to galactic structure and large scale
abundance gradients in the Galaxy. The observed starcounts in each field are a
good match to the predictions of models based on deep starcount data in other
intermediate-latitude fields, and these models identify the late-type stars as
members of the Galactic disk. Abundances for these late type stars are
estimated via narrowband indices that measure the strength of the TiO and CaH
bands in their spectra. Our results show that the average abundance in the
Galactic disk remains close to solar even at heights of more than 2 kpc above
the Plane.Comment: to appear in PASP; 17 pages, including 7 embedded, postscript figures
and 1 embedded table; uses AAS LaTeX style files (not included); also
available at http://astro.caltech.edu/~map/map.bibliography.htm
Contemporaneous XMM-Newton investigation of a giant X-ray flare and quiescent state from a cool M-class dwarf in the local cavity
We report the serendipitous detection of a giant X-ray flare from the source
2XMM J043527.2-144301 during an XMM-Newton observation of the high latitude
molecular cloud MBM20. The source has not been previously studied at any
wavelength. The X-ray flux increases by a factor of more than 52 from quiescent
state to peak of flare. A 2MASS counterpart has been identified (2MASS
J04352724-1443017), and near-infrared colors reveal a spectral type of M8-M8.5
and a distance of (67\pm 13) pc, placing the source in front of MBM20. Spectral
analysis and source luminosity are also consistent with this conclusion. The
measured distance makes this object the most distant source (by about a factor
of 4) at this spectral type detected in X-rays. The X-ray flare was
characterized by peak X-ray luminosity of ~8.2E28 erg s-1 and integrated X-ray
energy of ~2.3E32 erg. The flare emission has been characterized with a
2-temperature model with temperatures of ~10 and 46 MK (0.82 and 3.97 keV), and
is dominated by the higher temperature component.Comment: 19 pages, 5 figures; Accepted for publication on Ap
CORMASS: A Compact and Efficient NIR Spectrograph for Studying Low-Mass Objects
CorMASS (Cornell Massachusetts Slit Spectrograph) is a compact,
low-resolution (R=300), double-pass prism cross-dispersed near-infrared (NIR)
spectrograph in operation on the Palomar Observatory 60-inch telescope. Its
2-dimensional spectral format provides simultaneous coverage from lambda ~ 0.75
microns to lambda ~ 2.5 microns (z'JHK bands). A remotely operated cold flip
mirror permits its NICMOS3 detector to function as a K_s slit viewer to assist
object placement into the 2 arcsec x 15 arcsec slit. CorMASS was primarily
designed for the rapid spectral classification of low-mass stellar and
sub-stellar objects identified by the Two-Micron All Sky Survey (2MASS).
CorMASS' efficiency and resolution also make it a versatile instrument for the
spectral observation and classification of many other types of bright objects
(K<14) including quasars, novae, and emission line objects.Comment: To be published in Feb 2001 PASP, 19 pages, 12 Figures, High
Resolution file can be retrieved from
ftp://iras2.tn.cornell.edu/pub/wilson/papers/cormass.ps.g
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