The remnant of SN 1987A revealed at (sub-)mm wavelengths

Lakićević, M.; Loon, Jacco Th. van; Patat, F.; Zanardo, Giovanna

doi:10.1051/0004-6361/201116978

Cited by 15 publications

(30 citation statements)

References 18 publications

(46 reference statements)

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“…(a) Arnett et al (1989); (b) Krause et al (2008); (c) Eriksen et al (2009); (d) Smith (2013); (e) MacAlpine & Satterfield (2008); ( f ) Matsuura et al (2011); (g) Indebetouw et al (2014); (h) Lakićević et al (2011); (i) Barlow et al (2010); ( j) Rho et al (2008); (k) Dunne et al (2009); (l) Gomez et al (2012); (m) Park et al (2012); (n) Otsuka et al (2010).…”

Section: Referencesmentioning

confidence: 99%

Dust grains from the heart of supernovae

Bocchio

Marassi

Schneider

et al. 2016

A&A

141

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Dust grains are classically thought to form in the winds of asymptotic giant branch (AGB) stars. However, there is increasing evidence today for dust formation in supernovae (SNe). To establish the relative importance of these two classes of stellar sources of dust, it is important to know the fraction of freshly formed dust in SN ejecta that is able to survive the passage of the reverse shock and be injected in the interstellar medium. With this aim, we have developed a new code, GRASH_Rev, that allows following the dynamics of dust grains in the shocked SN ejecta and computing the time evolution of the mass, composition, and size distribution of the grains. We considered four well-studied SNe in the Milky Way and Large Magellanic Cloud: SN 1987A, CasA, the Crab nebula, and N49. These sources have been observed with both Spitzer and Herschel, and the multiwavelength data allow a better assessment the mass of warm and cold dust associated with the ejecta. For each SN, we first identified the best explosion model, using the mass and metallicity of the progenitor star, the mass of 56 Ni, the explosion energy, and the circumstellar medium density inferred from the data. We then ran a recently developed dust formation model to compute the properties of freshly formed dust. Starting from these input models, GRASH_Rev self-consistently follows the dynamics of the grains, considering the effects of the forward and reverse shock, and allows predicting the time evolution of the dust mass, composition, and size distribution in the shocked and unshocked regions of the ejecta. All the simulated models aagree well with observations. Our study suggests that SN 1987A is too young for the reverse shock to have affected the dust mass. Hence the observed dust mass of 0.7−0.9 M in this source can be safely considered as indicative of the mass of freshly formed dust in SN ejecta. Conversely, in the other three SNe, the reverse shock has already destroyed between 10−40% of the initial dust mass. However, the largest dust mass destruction is predicted to occur between 10 3 and 10 5 yr after the explosions. Since the oldest SN in the sample has an estimated age of 4800 yr, current observations can only provide an upper limit to the mass of SN dust that will enrich the interstellar medium, the so-called effective dust yields. We find that only between 1−8% of the currently observed mass will survive, resulting in an average SN effective dust yield of (1.55 ± 1.48) × 10 −2 M . This agrees well with the values adopted in chemical evolution models that consider the effect of the SN reverse shock. We discuss the astrophysical implications of our results for dust enrichment in local galaxies and at high redshift.

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Section: Referencesmentioning

confidence: 99%

Dust grains from the heart of supernovae

Bocchio

Marassi

Schneider

et al. 2016

A&A

141

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“…The reduction procedures included application of uniform weighting, one iteration of phase self-calibration over 1 http://www.atnf.csiro.au/computing/software/miriad Lakićević et al (2011Lakićević et al ( , 2012, Zanardo et al (2010), and this work. Power laws are fitted to λ > 30 cm, and two different models for dust emission are plotted (cf.…”

Section: Observations and Data Reductionmentioning

confidence: 99%

“…6 in diameter is linked to mass loss from the progenitor star (Bouchet et al 2006;Dwek et al 2010). Recently, Matsuura et al (2011) detected a second dust component, of only ≈18 K, which is also seen at 0.87 mm wavelength (Lakićević et al 2011). Matsuura et al argued that the cold dust had formed in the ejecta of The processed data are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/541/L2 SN 1987A.…”

Section: Introductionmentioning

confidence: 99%

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The remnant of supernova 1987A resolved at 3-mm wavelength

Lakićević

Zanardo

Loon

et al. 2012

A&A

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Context. The proximity of core-collapse supernova 1987A (SN 1987A) in the Large Magellanic Cloud (LMC) and its rapid evolution make it a unique case study of the development of a young supernova remnant. Aims. We aim at resolving the remnant of SN 1987A for the first time in the 3-mm band (at 94 GHz). Methods. We observed the source at 3-mm wavelength with a 750-m configuration of the Australia Telescope Compact Array (ATCA). We compared the image with a recent 3-cm image and with archival X-ray images.Results. We present a diffraction-limited image with a resolution of 0. 7, revealing the ring structure seen at lower frequencies and at other wavebands. The emission peaks in the eastern part of the ring. The 3-mm image bears resemblance to early X-ray images (from 1999-2000). We place an upper limit of 1 mJy (2σ) on any discrete source of emission in the centre (inside of the ring). The integrated flux density at 3 mm has doubled over the six years since the previous observations at 3 mm. Conclusions. At 3 mm -i.e. within the operational domain of the Atacama Large Millimeter/submillimeter Array (ALMA) -SN 1987A appears to be dominated by synchrotron radiation from the inner rim of the equatorial ring, characterised by moderately weak shocks. There is no clear sign of emission of a different nature, but the current limits do not rule out such component altogether.

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“…However, many recent studies derive low efficiencies of dust condensation in SN ejecta from mid-and far-IR observations (e.g., Ercolano et al 2007;Rho et al 2008Rho et al , 2009Temim et al 2012), theoretical modelling of dust formation and survival in SN ejecta (Bianchi & Schneider 2007;Kozasa et al 2009;Cherchneff & Dwek 2009, and analysis of presolar grains with different origins found in meteorites . Recently, far-IR and submillimeter observations with the Herschel Space Observatory permitted the detection of larger masses of newly formed dust in SN ejecta (Matsuura et al 2011;Gomez et al 2012; see also Lakicevic et al 2011, for ground-based sub-mm observations), but it is still unclear what fraction of these grains will survive destruction in the reverse shocks of SN remnants (e.g., Silvia et al 2010Silvia et al , 2012. Given the controversies with dust input from SNe, AGB stars may be a dominant stellar source of dust production.…”

Section: Introductionmentioning

confidence: 99%

Dust input from AGB stars in the Large Magellanic Cloud

Zhukovska

Henning

2013

A&A

112

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Aims. The dust-forming population of AGB stars and their input to the interstellar dust budget of the Large Magellanic Cloud (LMC) are studied with evolutionary dust models with the main goals (1) to investigate how the amount and composition of dust from AGB stars vary over the galactic history; (2) to characterise the mass and metallicity distribution of the present population of AGB stars; (3) to quantify the contribution of AGB stars of different mass and metallicity to the present stardust population in the interstellar medium (ISM). Methods. We used models of the stardust lifecycle in the ISM developed and tested for the solar neighbourhood. The first global spatially resolved reconstruction of the star formation history of the LMC from the Magellanic Clouds Photometric Survey was employed to calculate the stellar populations in the LMC. Results. The dust input from AGB stars is dominated by carbon grains from stars with masses 4 M almost during the entire history of the LMC. The production of silicate, silicon carbide, and iron dust is delayed until the ISM is enriched to about half the present metallicity in the LMC. For the first time, theoretically calculated dust production rates of AGB stars are compared with those derived from infrared observations of AGB stars for the entire galaxy. We find good agreement within scatter of various observational estimates. We show that the majority of silicate and iron grains in the present stardust population originate from a small population of intermediate-mass stars consisting of only 4% of the total number of stars, whereas in the solar neighbourhood they originate from low-mass stars. With models of the lifecycle of stardust grains in the ISM we confirm the strong discrepancy between dust input from stars and the existing interstellar dust mass in the LMC reported previously.

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The remnant of SN 1987A revealed at (sub-)mm wavelengths

Cited by 15 publications

References 18 publications

Dust grains from the heart of supernovae

Dust grains from the heart of supernovae

The remnant of supernova 1987A resolved at 3-mm wavelength

Dust input from AGB stars in the Large Magellanic Cloud

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