skip to main content
OSTI.GOV title logo U.S. Department of Energy
Office of Scientific and Technical Information

Title: First Scattered-light Images of the Gas-rich Debris Disk around 49 Ceti

Abstract

We present the first scattered-light images of the debris disk around 49 Ceti, a ∼40 Myr A1 main-sequence star at 59 pc, famous for hosting two massive dust belts as well as large quantities of atomic and molecular gas. The outer disk is revealed in reprocessed archival Hubble Space Telescope NICMOS-F110W images, as well as new coronagraphic H-band images from the Very Large Telescope SPHERE instrument. The disk extends from 1.″1 (65 au) to 4.″6 (250 au) and is seen at an inclination of 73°, which refines previous measurements at lower angular resolution. We also report no companion detection larger than 3 M {sub Jup} at projected separations beyond 20 au from the star (0.″34). Comparison between the F110W and H-band images is consistent with a gray color of 49 Ceti’s dust, indicating grains larger than ≳2 μ m. Our photometric measurements indicate a scattering efficiency/infrared excess ratio of 0.2–0.4, relatively low compared to other characterized debris disks. We find that 49 Ceti presents morphological and scattering properties very similar to the gas-rich HD 131835 system. From our constraint on the disk inclination we find that the atomic gas previously detected in absorption must extend to the inner disk, andmore » that the latter must be depleted of CO gas. Building on previous studies, we propose a schematic view of the system describing the dust and gas structure around 49 Ceti and hypothetical scenarios for the gas nature and origin.« less

Authors:
 [1]; ;  [2]; ; ;  [3];  [4];  [5];  [6];  [7];  [8];  [9];
  1. Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109 (United States)
  2. European Southern Observatory, Alonso de Còrdova 3107, Vitacura, Casilla 19001, Santiago (Chile)
  3. Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218 (United States)
  4. Exoplanets and Stellar Astrophysics Laboratory, NASA Goddard Space Flight Center, Code 667, Greenbelt, MD 20771 (United States)
  5. Univ. Grenoble Alpes, CNRS, IPAG, F-38000 Grenoble (France)
  6. Astrophysikalisches Institut und Universitätssternwarte, Friedrich-Schiller-Universität Jena, Schillergäßchen 2-3, D-07745 Jena (Germany)
  7. Space sciences, Technologies and Astrophysics Research (STAR) Institute, Université de Liège, 19 Allée du Six Août, B-4000 Liège (Belgium)
  8. LESIA, Observatoire de Paris, PSL Research University, CNRS, Sorbonne Universités, UPMC Univ. Paris 06, Univ. Paris Diderot, Sorbonne Paris Cité, 5 place Jules Janssen, F-92195 Meudon (France)
  9. Instituto Nacional de Astrofísica, Óptica y Electrónica, Luis Enrique Erro 1, Sta. Ma. Tonantzintla, Puebla (Mexico)
Publication Date:
OSTI Identifier:
22654577
Resource Type:
Journal Article
Resource Relation:
Journal Name: Astrophysical Journal Letters; Journal Volume: 834; Journal Issue: 2; Other Information: Country of input: International Atomic Energy Agency (IAEA)
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; ABSORPTION; CARBON; CARBON MONOXIDE; COMPARATIVE EVALUATIONS; DUSTS; IMAGE PROCESSING; IMAGES; LIMITING VALUES; MAIN SEQUENCE STARS; RESOLUTION; SCATTERING; SPACE; TELESCOPES; VISIBLE RADIATION

Citation Formats

Choquet, Élodie, Milli, Julien, Wahhaj, Zahed, Soummer, Rémi, Chen, Christine H., Debes, John H., Roberge, Aki, Augereau, Jean-Charles, Booth, Mark, Absil, Olivier, Boccaletti, Anthony, Burgo, Carlos del, E-mail: echoquet@jpl.nasa.gov, and and others. First Scattered-light Images of the Gas-rich Debris Disk around 49 Ceti. United States: N. p., 2017. Web. doi:10.3847/2041-8213/834/2/L12.
Choquet, Élodie, Milli, Julien, Wahhaj, Zahed, Soummer, Rémi, Chen, Christine H., Debes, John H., Roberge, Aki, Augereau, Jean-Charles, Booth, Mark, Absil, Olivier, Boccaletti, Anthony, Burgo, Carlos del, E-mail: echoquet@jpl.nasa.gov, & and others. First Scattered-light Images of the Gas-rich Debris Disk around 49 Ceti. United States. doi:10.3847/2041-8213/834/2/L12.
Choquet, Élodie, Milli, Julien, Wahhaj, Zahed, Soummer, Rémi, Chen, Christine H., Debes, John H., Roberge, Aki, Augereau, Jean-Charles, Booth, Mark, Absil, Olivier, Boccaletti, Anthony, Burgo, Carlos del, E-mail: echoquet@jpl.nasa.gov, and and others. Tue . "First Scattered-light Images of the Gas-rich Debris Disk around 49 Ceti". United States. doi:10.3847/2041-8213/834/2/L12.
@article{osti_22654577,
title = {First Scattered-light Images of the Gas-rich Debris Disk around 49 Ceti},
author = {Choquet, Élodie and Milli, Julien and Wahhaj, Zahed and Soummer, Rémi and Chen, Christine H. and Debes, John H. and Roberge, Aki and Augereau, Jean-Charles and Booth, Mark and Absil, Olivier and Boccaletti, Anthony and Burgo, Carlos del, E-mail: echoquet@jpl.nasa.gov and and others},
abstractNote = {We present the first scattered-light images of the debris disk around 49 Ceti, a ∼40 Myr A1 main-sequence star at 59 pc, famous for hosting two massive dust belts as well as large quantities of atomic and molecular gas. The outer disk is revealed in reprocessed archival Hubble Space Telescope NICMOS-F110W images, as well as new coronagraphic H-band images from the Very Large Telescope SPHERE instrument. The disk extends from 1.″1 (65 au) to 4.″6 (250 au) and is seen at an inclination of 73°, which refines previous measurements at lower angular resolution. We also report no companion detection larger than 3 M {sub Jup} at projected separations beyond 20 au from the star (0.″34). Comparison between the F110W and H-band images is consistent with a gray color of 49 Ceti’s dust, indicating grains larger than ≳2 μ m. Our photometric measurements indicate a scattering efficiency/infrared excess ratio of 0.2–0.4, relatively low compared to other characterized debris disks. We find that 49 Ceti presents morphological and scattering properties very similar to the gas-rich HD 131835 system. From our constraint on the disk inclination we find that the atomic gas previously detected in absorption must extend to the inner disk, and that the latter must be depleted of CO gas. Building on previous studies, we propose a schematic view of the system describing the dust and gas structure around 49 Ceti and hypothetical scenarios for the gas nature and origin.},
doi = {10.3847/2041-8213/834/2/L12},
journal = {Astrophysical Journal Letters},
number = 2,
volume = 834,
place = {United States},
year = {Tue Jan 10 00:00:00 EST 2017},
month = {Tue Jan 10 00:00:00 EST 2017}
}