ALMA observations of the Red Rectangle, a preliminary analysis

Bujarrabal, V.; Castro-Carrizo, A.; Alcolea, J.; Winckel, H. Van; Contreras, C. Sánchez; Santander-García, M.; Neri, R.; Lucas, R.

doi:10.1051/0004-6361/201322232

Cited by 57 publications

(107 citation statements)

References 12 publications

(12 reference statements)

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“…The total mass in the ring, ∼ 0.06M , is much smaller than any mass ejected in the CE process that shrank the binary orbit. A somewhat similar structure of bipolar nebulae and a ring is seen around post-AGB stars (Bujarrabal et al 2013a), e.g., the Red Rectangle (Cohen et al 2004;Bujarrabal et al 2013b). However, in the Red Rectangle the ring is in a Keplerian rotation (Jura et al 1995), there is an outflowing disk, and the secondary star did not enter a CE phase (van Winckel 2003).…”

Section: Introductionmentioning

confidence: 70%

Forming equatorial rings around dying stars

Akashi

Sabach

Yogev

et al. 2015

Mon. Not. R. Astron. Soc.

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We suggest that clumpy-dense outflowing equatorial rings around evolved giant stars, such as in supernova 1987A and the Necklace planetary nebula, are formed by bipolar jets that compress gas toward the equatorial plane. The jets are launched from an accretion disk around a stellar companion. Using the FLASH hydrodynamics numerical code we perform 3D numerical simulations, and show that bipolar jets expanding into a dense spherical shell can compress gas toward the equatorial plane and lead to the formation of an expanding equatorial ring. RayleighTaylor instabilities in the interaction region break the ring to clumps. Under the assumption that the same ring-formation mechanism operates in massive stars and in planetary nebulae, we find this mechanism to be more promising for ring formation than mass loss through the second Lagrangian point. The jets account also for the presence of a bipolar nebula accompanying many of the rings.

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Section: Introductionmentioning

confidence: 70%

Forming equatorial rings around dying stars

Akashi

Sabach

Yogev

et al. 2015

Mon. Not. R. Astron. Soc.

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“…Another Band 9 project used continuum observations of SN1987A to conclude that such supernovae may be cosmologically important producers of dust Zanardo et al 2014). In the field of evolved stars, Bujarrabal et al (2013) included observations of 12 CO 6-5 in their analysis of the gas kinematics of the post-AGB object the Red Rectangle. Recently, Decin et al (2015) used Band 9 to reveal the presence of spiral structure in the inner wind of CW Leo.…”

Section: Early Science Results Using Band 9 Observationsmentioning

confidence: 99%

The ALMA Band 9 receiver

Baryshev

Hesper

Mena

et al. 2015

A&A

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Aims. We describe the design, construction, and characterization of the Band 9 heterodyne receivers (600-720 GHz) for the Atacama Large Millimeter/submillimeter Array (ALMA). First-light Band 9 data, obtained during ALMA commissioning and science verification phases, are presented as well. Methods. The ALMA Band 9 receiver units (so-called "cartridges"), which are installed in the telescope's front end, have been designed to detect and down-convert two orthogonal linear polarization components of the light collected by the ALMA antennas. The light entering the front end is refocused with a compact arrangement of mirrors, which is fully contained within the cartridge. The arrangement contains a grid to separate the polarizations and two beam splitters to combine each resulting beam with a local oscillator signal. The combined beams are fed into independent double-sideband mixers, each with a corrugated feedhorn coupling the radiation by way of a waveguide with backshort cavity into an impedance-tuned superconductor-insulator-superconductor (SIS) junction that performs the heterodyne down-conversion. Finally, the generated intermediate frequency (IF) signals are amplified by cryogenic and room-temperature HEMT amplifiers and exported to the telescope's IF back end for further processing and, finally, correlation. Results. The receivers have been constructed and tested in the laboratory and they show an excellent performance, complying with ALMA requirements. Performance statistics on all 73 Band 9 receivers are reported. Importantly, two different tunnel-barrier technologies (necessitating different tuning circuits) for the SIS junctions have been used, namely conventional AlO x barriers and the more recent high-current-density AlN barriers. On-sky characterization and tests of the performance of the Band 9 cartridges are presented using commissioning data. Continuum and line images of the low-mass protobinary IRAS 16293-2422 are presented which were obtained as part of the ALMA science verification program. An 8 GHz wide Band 9 spectrum extracted over a 0.3 × 0.3 region near source B, containing more than 100 emission lines, illustrates the quality of the data.

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“…L 2 Puppis (HD 56096, HIP 34922, HR 2748) is an asymptotic giant branch (AGB) semiregular variable. Its variability was discovered by Gould as early as 1872 (Cannon 1907). Its M5III spectral type corresponds to an approximate effective temperature of T eff = 3500 K, which is what we considered here.…”

Section: Introductionmentioning

confidence: 82%

“…in MyCn 18 by Sahai et al 1999), and in the millimeter domain (e.g. in the Red Rectangle by Bujarrabal et al 2013b). These objects present a remarkable axial symmetry, whose origin is often attributed to the presence of a central disk.…”

Section: Mass-loss Geometrymentioning

confidence: 99%

An edge-on translucent dust disk around the nearest AGB star, L₂Puppis

Kervella

Montargès

Ridgway

et al. 2014

A&A

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As the nearest known AGB star (d = 64 pc) and one of the brightest (m K ≈ −2), L 2 Pup is a particularly interesting benchmark object to monitor the final stages of stellar evolution. We report new serendipitous imaging observations of this star with the VLT/NACO adaptive optics system in twelve narrow-band filters covering the 1.0−4.0 µm wavelength range. These diffraction-limited images reveal an extended circumstellar dust lane in front of the star that exhibits a high opacity in the J band and becomes translucent in the H and K bands. In the L band, extended thermal emission from the dust is detected. We reproduced these observations using Monte Carlo radiative transfer modeling of a dust disk with the RADMC-3D code. We also present new interferometric observations with the VLTI/VINCI and MIDI instruments. We measured in the K band an upper limit to the limb-darkened angular diameter of θ LD = 17.9 ± 1.6 mas, converting to a maximum linear radius of R = 123 ± 14 R . Considering the geometry of the extended K band emission in the NACO images, this upper limit is probably close to the actual angular diameter of the star. The position of L 2 Pup in the Hertzsprung-Russell diagram indicates that this star has a mass of about 2 M and is probably experiencing an early stage of the asymptotic giant branch. We did not detect any stellar companion of L 2 Pup in our adaptive optics and interferometric observations, and we attribute its apparent astrometric wobble in the H data to variable lighting effects on its circumstellar material. However, we do not exclude the presence of a binary companion, because the large loop structure extending to more than 10 AU to the northeast of the disk in our L-band images may be the result of interaction between the stellar wind of L 2 Pup and a hidden secondary object. The geometric configuration that we propose, with a large dust disk seen almost edge-on, appears particularly favorable to test and develop our understanding of the formation of bipolar nebulae.

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ALMA observations of the Red Rectangle, a preliminary analysis

Cited by 57 publications

References 12 publications

Forming equatorial rings around dying stars

Forming equatorial rings around dying stars

The ALMA Band 9 receiver

An edge-on translucent dust disk around the nearest AGB star, L₂Puppis

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ALMA observations of the Red Rectangle, a preliminary analysis

Cited by 57 publications

References 12 publications

Forming equatorial rings around dying stars

Forming equatorial rings around dying stars

The ALMA Band 9 receiver

An edge-on translucent dust disk around the nearest AGB star, L2Puppis

Contact Info

Product

Resources

About

An edge-on translucent dust disk around the nearest AGB star, L₂Puppis