105 research outputs found
On the Interferometric Sizes of Young Stellar Objects
Long-baseline optical interferometers can now detect and resolve hot dust
emission thought to arise at the inner edge of circumstellar disks around young
stellar objects (YSOs). We argue that the near-infrared sizes being measured
are closely related to the radius at which dust is sublimated by the stellar
radiation field. We consider how realistic dust optical properties and gas
opacity dramatically affect the predicted location of this dust destruction
radius, an exercise routinely done in other contexts but so far neglected in
the analysis of near-infrared sizes of YSOs. We also present the accumulated
literature of near-infrared YSO sizes in the form of a ``size-luminosity
diagram'' and compare with theoretical expectations. We find evidence that
large (>~ 1 micron) dust grains predominate in the inner disks of T Tauri and
Herbig Ae/Be stars, under the assumption that the inner-most gaseous disks are
optically-thin at visible wavelengths.Comment: Accepted by Astrophysical Journa
JouFLU: upgrades to the Fiber Linked Unit for Optical Recombination (FLUOR) interferometric beam combiner
The Fiber Linked Unit for Optical Recombination (FLUOR) is a precision interferometric beam combiner operating at the CHARA Array on Mt. Wilson, CA. It has recently been upgraded as part of a mission known as “Jouvence of FLUOR” or JouFLU. As part of this program JouFLU has new mechanic stages and optical payloads, new alignment systems, and new command/control software. Furthermore, new capabilities have been implemented such as a Fourier Transform Spectrograph (FTS) mode and spectral dispersion mode. These upgrades provide new capabilities to JouFLU as well as improving statistical precision and increasing observing efficiency. With these new systems, measurements of interferometric visibility to the level of 0.1% precision are expected on targets as faint as 6th magnitude in the K band. Here we detail the upgrades of JouFLU and report on its current status
Study of molecular layers in the atmosphere of the supergiant star µ Cep by interferometry in the K band
Infrared interferometry of supergiant and Mira stars has recently been reinterpreted as revealing the presence of deep molecular layers. Empirical models for a photosphere surrounded by a simple molecular layer or envelope have led to a consistent interpretation of previously inconsistent data. The stellar photospheres are found to be smaller than previously understood, and the molecular layer is much higher and denser than predicted by hydrostatic equilibrium. However, the analysis was based on spatial observations with medium-band optical filters, which mixed the visibilities of different spatial structures. This paper reports spatial interferometry with narrow spectral bands, isolating near-continuum and strong molecular features, obtained for the supergiant µ Cep. The measurements confirm strong variation of apparent diameter across the K-band. A layer model shows that a stellar photosphere of angular diameter 14.11±0.60 mas is surrounded by a molecular layer of diameter 18.56±0.26 mas, with an optical thickness varying from nearly zero at 2.15 µm to >1 at 2.39 µm. Although µ Cep and α Ori have a similar spectral type, interferometry shows that they differ in their radiative properties. Comparison with previous broad-band measurements shows the importance of narrow spectral bands. The molecular layer or envelope appears to be a common feature of cool supergiants
Probing the close environment of young stellar objects with interferometry
The study of Young Stellar Objects (YSOs) is one of the most exciting topics
that can be undertaken by long baseline optical interferometry. The magnitudes
of these objects are at the edge of capabilities of current optical
interferometers, limiting the studies to a few dozen, but are well within the
capability of coming large aperture interferometers like the VLT
Interferometer, the Keck Interferometer, the Large Binocular Telescope or
'OHANA. The milli-arcsecond spatial resolution reached by interferometry probes
the very close environment of young stars, down to a tenth of an astronomical
unit. In this paper, I review the different aspects of star formation that can
be tackled by interferometry: circumstellar disks, multiplicity, jets. I
present recent observations performed with operational infrared
interferometers, IOTA, PTI and ISI, and I show why in the next future one will
extend these studies with large aperture interferometers.Comment: Review to be published in JENAM'2002 proceedings "The Very Large
Telescope Interferometer Challenges for the future
Co-phasing the Large Binocular Telescope: status and performance of LBTI/PHASECam
The Large Binocular Telescope Interferometer is a NASA-funded nulling and
imaging instrument designed to coherently combine the two 8.4-m primary mirrors
of the LBT for high-sensitivity, high-contrast, and high-resolution infrared
imaging (1.5-13 um). PHASECam is LBTI's near-infrared camera used to measure
tip-tilt and phase variations between the two AO-corrected apertures and
provide high-angular resolution observations. We report on the status of the
system and describe its on-sky performance measured during the first semester
of 2014. With a spatial resolution equivalent to that of a 22.8-meter telescope
and the light-gathering power of single 11.8-meter mirror, the co-phased LBT
can be considered to be a forerunner of the next-generation extremely large
telescopes (ELT).Comment: 8 pages, 5 figures, SPIE Conference proceeding
Study of molecular layers in the atmosphere of the supergiant star mu Cep by interferometry in the K band
Infrared interferometry of supergiant and Mira stars has recently been
reinterpreted as revealing the presence of deep molecular layers. Empirical
models for a photosphere surrounded by a simple molecular layer or envelope
have led to a consistent interpretation of previously inconsistent data. The
stellar photospheres are found to be smaller than previously understood, and
the molecular layer is much higher and denser than predicted by hydrostatic
equilibrium. However, the analysis was based on spatial observations with
medium-band optical filters, which mixed the visibilities of different spatial
structures. This paper reports spatial interferometry with narrow spectral
bands, isolating near-continuum and strong molecular features, obtained for the
supergiant mu Cep. The measurements confirm strong variation of apparent
diameter across the K-band. A layer model shows that a stellar photosphere of
angular diameter 14.11+/-0.60 mas is surrounded by a molecular layer of
diameter 18.56+/-0.26 mas, with an optical thickness varying from nearly zero
at 2.15 microns to >1 at 2.39 microns. Although mu Cep and alpha Ori have a
similar spectral type, interferometry shows that they differ in their radiative
properties. Comparison with previous broad-band measurements shows the
importance of narrow spectral bands. The molecular layer or envelope appears to
be a common feature of cool supergiants.Comment: 9 pages, 2 figures, to appear in A&
Aperture synthesis using multiple facilities: Keck aperture masking and the IOTA interferometer
As the number of optical interferometers increase, multi-facility observations become both feasible and scientifically interesting. For imaging of complex sources, the capability of increasing (u,v) coverage by using multiple arrays may be necessary for accurately interpreting the fringe visibility and closure phase data. Toward this end, coordinated observations with the IOTA interferometer and Keck aperture masking have been carried out to test techniques for synthesizing images using data from heterogeneous arrays with sparse (u,v) coverage. In particular, we will focus on how the image prior in the Maximum Entropy Method can be used to efficiently incorporate very high spatial frequency information with "low-resolution" data for imaging the generic prototype "Star + Dust Shell" image morphology. Preliminary results using real data for a few dusty evolved stars are presented
Exoplanet science with the LBTI: instrument status and plans
The Large Binocular Telescope Interferometer (LBTI) is a strategic instrument
of the LBT designed for high-sensitivity, high-contrast, and high-resolution
infrared (1.5-13 m) imaging of nearby planetary systems. To carry out a
wide range of high-spatial resolution observations, it can combine the two
AO-corrected 8.4-m apertures of the LBT in various ways including direct
(non-interferometric) imaging, coronagraphy (APP and AGPM), Fizeau imaging,
non-redundant aperture masking, and nulling interferometry. It also has
broadband, narrowband, and spectrally dispersed capabilities. In this paper, we
review the performance of these modes in terms of exoplanet science
capabilities and describe recent instrumental milestones such as first-light
Fizeau images (with the angular resolution of an equivalent 22.8-m telescope)
and deep interferometric nulling observations.Comment: 12 pages, 6 figures, Proc. SPI
Recent science results with the two-telescope IOTA
The IOTA (Infrared Optical Telescope Array) has been routinely operating with two-telescopes since 1994, a mode destined to become obsolete following its recent conversion to a three-telescope array. In two-telescope mode, the IOTA has made numerous scientific and technical contributions, see e.g. our list of publications at http://cfa-www.harvard.edu/cfa/oir/IOTA/PUBLI/publications.html. We present preliminary results on three different topics using recent data from the two-telescope IOTA: (1) measurements of Mira star diameters simultaneously in three different near-infrared spectral bands, (2) measurement of the characteristic size and shape of the source of near-infared emission in the x-ray binary system CI Cam, and (3) aperture synthesis of the Carbon star V Hydrae combining data from the IOTA and from aperture masking at the Keck-I telescope
The physical conditions in Gomez's Hamburger (IRAS 18059-3211), a pre-MS rotating disk
We aim to study the structure, dynamics and physical conditions of Gomez's
Hamburger (IRAS 18059-3211; GoHam). We confirm that GoHam essentially consists
of a flaring disk in keplerian rotation around a young, probably pre-MS star.
We present high resolution SMA maps of 12CO J=2-1, 13CO J=2-1, 12CO J=3-2, and
C17O J=3-2, as well as data on 12CO J=6-5 and the continuum flux at these
wavelengths. Spatial resolutions up to 1" are obtained. Except for the C17O
data, the dynamical ranges are larger than 10. The maps are compared to a
numerical model, which simulates the emission of a rotating disk with the
expected general properties of such objects; a very satisfactory fitting of our
maps is obtained. The meaning and reliability of our results are thoroughly
discussed. Our observations allow measurement of the main properties of GoHam
at scales between ~ 1" (~ 5 10^15 cm, for the assumed distance, 300 pc) and the
total extent of the nebula, 14". We are able to measure the global structure of
the gas-rich disk, which is found to be flaring, and its dynamics, which is
clearly dominated by keplerian rotation, with a very small degree of
turbulence. The combination of different lines, particularly showing different
opacities, allows us to reasonably estimate the distributions of the gas
temperature and density. We clearly find a significant and sharp increase in
temperature at large distances from the equator, accompanied by a decrease in
density of the same order. Finally, we identify and study a condensation in the
southern part of the disk that has no counterparts in the rest of the nebula.
This condensation is quite extended (about 5 10^15 cm), contains a significant
amount of mass (roughly, ~ 6 10^-3 Mo), and seems to be associated with a
detectable distortion of the global rotation kinematics.Comment: 16 pages, 12 figures, 1 pdflatex text file, goha.bbl file, aa.cls
style fil
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