John M. Carpenter

Atacama Large Millimeter Submillimeter Array

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Co-Authors

Lynne A. Hillenbrand

California Institute of Technology

105

Andrea Isella

Rice University

Sean M. Andrews

Center for Astrophysics Harvard & Smithsonian

Laura M. Pérez

University of Chile

David J. Wilner

Center for Astrophysics Harvard & Smithsonian

Luca Ricci

California State University, Northridge

Eric E. Mamajek

University of Rochester

Thomas Henning

Max Planck Institute for Astronomy

J. R. Stauffer

Mayo Clinic in Florida

L. Testi

Arcetri Astrophysical Observatory

Cooperative Institutions

California Institute of Technology

274

Center for Astrophysics Harvard & Smithsonian

205

Max Planck Society

203

Max Planck Institute for Astronomy

152

Centre National de la Recherche Scientifique

135

University of Arizona

132

Jet Propulsion Laboratory

127

Goddard Space Flight Center

126

Commissariat à l'Énergie Atomique et aux Énergies Alternatives

114

University of California, Berkeley

111

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Large-scale CO Spiral Arms and Complex Kinematics Associated with the T Tauri Star RU Lup

The Astrophysical Journal (2020)

Jane Huang Sean M. Andrews Karin I. Öberg Megan Ansdell M. Benisty

While protoplanetary disks often appear to be compact and well-organized in millimeter continuum emission, CO spectral line observations are increasingly revealing complex behavior at large distances from the host star. We present deep ALMA maps of the $J=2-1$ transition of $^{12}$CO, $^{13}$CO, and C$^{18}$O, as well as the $J=3-2$ transition of DCO$^+$, toward the T Tauri star RU Lup at a resolution of $\sim0.3''$ ($\sim50$ au). The CO isotopologue emission traces four major components of the RU Lup system: a compact Keplerian disk with a radius of $\sim120$ au, a non-Keplerian ``envelope-like'' structure surrounding the disk and extending to $\sim260$ au from the star, at least five blueshifted spiral arms stretching up to 1000 au, and clumps outside the spiral arms located up to 1500 au in projection from RU Lup. We comment on potential explanations for RU Lup's peculiar gas morphology, including gravitational instability, accretion of material onto the disk, or perturbation by another star. RU Lup's extended non-Keplerian CO emission, elevated stellar accretion rate, and unusual photometric variability suggest that it could be a scaled-down Class II analog of the outbursting FU Ori systems.

Submillimeter Array

10.3847/1538-4357/aba1e1

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Citations (29)

Development of an 'all-digital' IF chain

astro2010: The Astronomy and Astrophysics Decadal Survey (2009)

D. P. Woody David Hawkins D. C. Backer Dan Werthimer John M. Carpenter

Chain (unit)

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Citations (0)

Primordial Mass Segregation in Proto-cluster Cores

American Astronomical Society Meeting Abstracts (2007)

Laura M. Perez Munoz John M. Carpenter

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Citations (0)

Chemical Gradients in the Orion Molecular Cloud

Springer eBooks (1992)

H. Ungerechts Edwin A. Bergin John M. Carpenter P. Goldsmith William M. Irvine

Nyquist–Shannon sampling theorem

10.1007/978-94-011-2761-5_60

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Citations (1)

VizieR Online Data Catalog: 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)

VizieR Online Data Catalog (2003)

R. M. Cutri M. F. Skrutskie Schuyler D. Van Dyk C. A. Beichman John M. Carpenter

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Citations (123)

Super-fast Rotation in the OMC 2/FIR 6b Jet

The Astrophysical Journal (2021)

Yuko Matsushita Satoko Takahashi Shun Ishii Kohji Tomisaka Paul T. P. Ho

We present ALMA CO ($J$=2--1) and 1.3 mm continuum observations of the high-velocity jet associated with the FIR 6b protostar located in the Orion Molecular Cloud-2. We detect a velocity gradient along the short axis of the jet in both the red- and blue-shifted components. The position-velocity diagrams along the short axis of the red-shifted jet show a typical characteristic of a rotating cylinder. We attribute the velocity gradient in the red-shifted component to rotation of the jet. The rotation velocity ($>20\,\ \rm{km s^{-1}}$) and specific angular momentum ($>10^{22}\, \rm{cm^{2}\, s^{-1}}$) of the jet around FIR 6b are the largest among all jets in which rotation has been observed. By combining disk wind theory with our observations, the jet launching radius is estimated to be in the range of $2.18-2.96$\,au. The rapid rotation, large specific angular momentum, and a launching radius far from the central protostar can be explained by a magnetohydrodynamic disk wind that contributes to the angular momentum transfer in the late stages of protostellar accretion.

Protostar

Submillimeter Array

Position angle

Velocity gradient

10.3847/1538-4357/ac069f

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Citations (11)

DISCOVERY, PROGENITOR AND EARLY EVOLUTION OF A STRIPPED ENVELOPE SUPERNOVA iPTF13bvn

The Astrophysical Journal Letters (2013)

Y. Cao M. M. Kasliwal I. Arcavi A. Horesh P. J. Hancock

The intermediate Palomar Transient Factory reports our discovery of a young supernova, iPTF13bvn, in the nearby galaxy, NGC 5806 (22.5 Mpc). Our spectral sequence in the optical and infrared suggests a Type Ib classification. We identify a blue progenitor candidate in deep pre-explosion imaging within a 2σ error circle of 80 mas (8.7 pc). The candidate has an MB luminosity of −5.52 ± 0.39 mag and a B − I color of 0.25 ± 0.25 mag. If confirmed by future observations, this would be the first direct detection for a progenitor of a Type Ib. Fitting a power law to the early light curve, we find an extrapolated explosion date around 0.6 days before our first detection. We see no evidence of shock cooling. The pre-explosion detection limits constrain the radius of the progenitor to be smaller than a few solar radii. iPTF13bvn is also detected in centimeter and millimeter wavelengths. Fitting a synchrotron self-absorption model to our radio data, we find a mass-loading parameter of 1.3×1012 g cm−1. Assuming a wind velocity of 103 km s−1, we derive a progenitor mass-loss rate of 3 × 10−5 M☉ yr−1. Our observations, taken as a whole, are consistent with a Wolf–Rayet progenitor of the supernova iPTF13bvn.

Solar mass

Progenitor

10.1088/2041-8205/775/1/l7

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Citations (200)

MISALIGNMENT OF MAGNETIC FIELDS AND OUTFLOWS IN PROTOSTELLAR CORES

The Astrophysical Journal (2013)

Charles L. H. Hull R. L. Plambeck Alberto D. Bolatto Geoffrey C. Bower John M. Carpenter

We present results of 1.3 mm dust polarization observations toward 16 nearby, low-mass protostars, mapped with ~2.5" resolution at CARMA. The results show that magnetic fields in protostellar cores on scales of ~1000 AU are not tightly aligned with outflows from the protostars. Rather, the data are consistent with scenarios where outflows and magnetic fields are preferentially misaligned (perpendicular), or where they are randomly aligned. If one assumes that outflows emerge along the rotation axes of circumstellar disks, and that the outflows have not disrupted the fields in the surrounding material, then our results imply that the disks are not aligned with the fields in the cores from which they formed.

Protostar

Circumstellar disk

Low Mass

10.1088/0004-637x/768/2/159

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Citations (140)

Distribution of solids in the rings of the HD 163296 disk: a multiwavelength study

Astronomy and Astrophysics (2022)

Greta Guidi Andrea Isella L. Testi C. J. Chandler Hauyu Baobab Liu

Context. Observations at millimeter wavelengths of bright protoplanetary disks have shown the ubiquitous presence of structures such as rings and spirals in the continuum emission. The derivation of the underlying properties of the emitting material is nontrivial because of the complex radiative processes involved. Aims. In this paper we analyze new observations from the Atacama Large Millimeter/submillimeter Array (ALMA) and the Karl G. Jansky Very Large Array (VLA) at high angular resolution corresponding to 5 – 8 au to determine the dust spatial distribution and grain properties in the ringed disk of HD 163296. Methods. We fit the spectral energy distribution as a function of the radius at five wavelengths from 0.9 to 9 mm, using a simple power law and a physical model based on an analytic description of radiative transfer that includes isothermal scattering. We considered eight dust populations and compared the models' performance using Bayesian evidence. Results. Our analysis shows that the moderately high optical depth ( τ >1) at λ ≤ 1.3 mm in the dust rings artificially lower the millimeter spectral index, which should therefore not be considered as a reliable direct proxy of the dust properties and especially the grain size. We find that the outer disk is composed of small grains on the order of 200 µm with no significant difference between rings at 66 and 100 au and the adjacent gaps, while in the innermost ~30 au, larger grains (≥mm) could be present. We show that the assumptions on the dust composition have a strong impact on the derived surface densities and grain size. In particular, increasing the porosity of the grains to 80% results in a total dust mass about five times higher with respect to grains with 25% porosity. Finally, we find that the derived opacities as a function of frequency deviate from a simple power law and that grains with a lower porosity seem to better reproduce the observations of HD 163296. Conclusions. While we do not find evidence of differential trapping in the rings of HD 163296, our overall results are consistent with the postulated presence of giant planets affecting the dust temperature structure and surface density, and possibly originating a second-generation dust population of small grains.

Opacity

Spectral index

Isothermal process

Spectral energy distribution

10.1051/0004-6361/202142303

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Citations (28)

A High-resolution Optical Survey of Upper Sco: Evidence for Coevolution of Accretion and Disk Winds

The Astrophysical Journal (2023)

Min Fang Ilaria Pascucci Suzan Edwards Uma Gorti Lynne A. Hillenbrand

Abstract Magnetohydrodynamic (MHD) and photoevaporative winds are thought to play an important role in the evolution and dispersal of planet-forming disks. Here, we analyze high-resolution (Δ v ∼ 7 km s −1 ) optical spectra from a sample of 115 T Tauri stars in the ∼5–10 Myr Upper Sco association and focus on the [O i ] λ 6300 and H α lines to trace disk winds and accretion, respectively. Our sample covers a large range of spectral types and we divide it into warm (G0-M3) and cool (later than M3) to facilitate comparison with younger regions. We detect the [O i ] λ 6300 line in 45 out of 87 Upper Sco sources with protoplanetary disks and 32 out of 45 are accreting based on H α profiles and equivalent widths. All [O i ] λ 6300 Upper Sco profiles have low-velocity (centroid < −30 km s −1 ; low-velocity component (LVC)) emission and most (36/45) can be fit by a single Gaussian (SC). The single-component (SC) distribution of centroid velocities and FWHMs is consistent with MHD disk winds. We also find that the Upper Sco sample follows the same accretion luminosity−LVC [O i ] λ 6300 relation and the same anticorrelation between SC FWHM and Wide-field Infrared Survey Explorer W3-W4 spectral indices as the younger samples. These results indicate that accretion and disk winds coevolve and that, as inner disks clear out, wind emission arises further away from the star. Finally, our large spectral range coverage reveals that cool stars have larger FWHMs normalized by stellar mass than warm stars indicating that [O i ] λ 6300 emission arises closer in toward lower-mass/lower luminosity stars.

Spectral index

10.3847/1538-4357/acb2c9

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Citations (16)