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

Lakićević, M.; Zanardo, Giovanna; Loon, Jacco Th. van; Potter, Toby; Ng, C.‐Y.; Gaensler, B. M.

doi:10.1051/0004-6361/201218902

Cited by 20 publications

(28 citation statements)

References 21 publications

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“…The ring flux densities are shown in Fig. 5, along with previous measurements of the ring from ALMA and the Australia Telescope Compact Array (ATCA): 1.4 GHz, 18 GHz, 44 GHz ); 9 GHz ; 94 GHz (Lakićević et al 2012). As the frequency increases towards the submm and FIR, the contribution of the thermal ejecta emission to the total emission becomes more significant, so the ring emission at day 9280 was estimated from the total flux densities at 102, 213, 345, & 672 GHz by scaling and subtracting an ejecta model component in Fourier space based on the Band-9 ejecta flux density at each frequency .…”

Section: The Ringmentioning

confidence: 89%

“…The literature values for the total SN 1987A flux densities at various wavelengths are shown as grey hexagons, and represent the overall spectral energy distribution (SED) of the system. The total emission at 1.4 GHz, 18 GHz, 44 GHz (Zanardo et al 2013), 9 GHz , 94 GHz (Lakićević et al 2012), and 102 GHz ) is dominated by synchrotron emission from the ring. The total emission at 213, 345, & 672 GHz ), on the other hand, gradually consists of a higher and higher fraction of thermal emission until that is dominant in the submm Figure 5.…”

Section: Photometrymentioning

confidence: 99%

“…The three physical mechanisms primarily responsible for emission in the FIR-radio portion of the continuum are thermal IR greybody emission from dust (from the ejecta region - Matsuura et al 2011;Indebetouw et al 2014), nonthermal radio/mm synchrotron emission (from the ring -Manchester 2007; Potter et al 2009;Zanardo et al 2010;Lakićević et al 2012;Zanardo et al 2013;) and a lesser contribution from free-free mm/submm bremsstrahlung emission from hot ionized material (see Zanardo et al 2014 for a full review of the different components). In this Section we measure the photometry, analyze the emission from dust in the ejecta using the ALMA data, investigate the properties derived using a variety of dust models from the literature, and investigate the synchrotron emission in the ring.…”

Section: The Spectral Energy Distribution Of Sn 1987amentioning

confidence: 99%

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High Angular Resolution ALMA Images of Dust and Molecules in the SN 1987A Ejecta

Cigan

Matsuura

Gomez

et al. 2019

ApJ

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100

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We present high angular resolution (∼80 mas) ALMA continuum images of the SN 1987A system, together with CO J=2→1, J=6 → 5, and SiO J=5→4 to J=7 → 6 images, which clearly resolve the ejecta (dust continuum and molecules) and ring (synchrotron continuum) components. Dust in the ejecta is asymmetric and clumpy, and overall the dust fills the spatial void seen in Hα images, filling that region with material from heavier elements. The dust clumps generally fill the space where CO J=6→5 is fainter, tentatively indicating that these dust clumps and CO are locationally and chemically linked. In these regions, carbonaceous dust grains might have formed after dissociation of CO. The dust grains would have cooled by radiation, and subsequent collisions of grains with gas would also cool the gas, suppressing the CO J=6→5 intensity. The data show a dust peak spatially coincident with the molecular hole seen in previous ALMA CO J=2→1 and SiO J=5→4 images. That dust peak, combined with CO and SiO line spectra, suggests that the dust and gas could be at higher temperatures than the surrounding material, though higher density cannot be totally excluded. One of the possibilities is that a compact source provides additional heat at that location. Fits to the far-infraredmillimeter spectral energy distribution give ejecta dust temperatures of 18-23K. We revise the ejecta dust mass to M dust = 0.2 − 0.4M for carbon or silicate grains, or a maximum of < 0.7M for a mixture of grain species, using the predicted nucleosynthesis yields as an upper limit. ciganp@cardiff.ac.uk

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Section: The Ringmentioning

confidence: 89%

Section: Photometrymentioning

confidence: 99%

Section: The Spectral Energy Distribution Of Sn 1987amentioning

confidence: 99%

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High Angular Resolution ALMA Images of Dust and Molecules in the SN 1987A Ejecta

Cigan

Matsuura

Gomez

et al. 2019

ApJ

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100

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“…More recently Matsuura et al (2011) have from Herschel far-IR observations found evidence for a large dust mass, estimated to 0.4 − 0.7 M ⊙ , but could be up to 2.4 M ⊙ . The mass estimate is, however, highly dependent on the dust temperature and the mass could be several orders of magnitude lower if the temperature is higher than adopted by Matsuura et al (2011), as discussed from APEX observations by Lakićević et al (2012).…”

Section: Dustmentioning

confidence: 98%

Late Spectral Evolution of the Ejecta and Reverse Shock in Sn 1987a

Fransson

Larsson

Spyromilio³

et al. 2013

ApJ

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We present observations with VLT and HST of the broad emission lines from the inner ejecta and reverse shock of SN 1987A from 1999 Feb. until 2012 Jan. (days 4381 -9100 after explosion). We detect broad lines from Hα, Hβ, Mg I], Na I, [O I], [Ca II] and a feature at ∼ 9220Å. We identify the latter line with Mg II λλ 9218, 9244, which is most likely pumped by Lyα fluorescence. Hα, and Hβ both have a centrally peaked component, extending to ∼ 4500 km s −1 and a very broad component extending to 11, 000 km s −1 , while the other lines have only the central component. The low velocity component comes from unshocked ejecta, heated mainly by X-rays from the circumstellar environment, whereas the broad component comes from faster ejecta passing through the reverse shock, created by the collision with the circumstellar ring. The flux in Hα from the reverse shock has increased by a factor of 4 − 6 from 2000 to 2007. After that there is a tendency of flattening of the light curve, similar to what may be seen in soft X-rays and in the optical lines from the shocked ring. The core component seen in Hα, [Ca II] and Mg II has experienced a similar increase, which is consistent with that found from HST photometry. The ring-like morphology of the ejecta is explained as a result of the X-ray illumination, depositing energy outside of the core of the ejecta. The energy deposition of the external X-rays is calculated using explosion models for SN 1987A and we predict that the outer parts of the unshocked ejecta will continue to brighten because of this. We finally discuss evidence for dust in the ejecta from line asymmetries.

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“…Observations at higher frequencies (18, 36, 44 and 94 GHz) undertaken with ATCA (Manchester et al 2005;Potter et al 2009;Lakićević et al 2012;Zanardo et al 2013), followed by observations at 110, 215, and 345 GHz with the Atacama Millimeter/Submillimeter Array (ALMA), show the same asymmetric double lobe morphology Zanardo et al 2014). Also ALMA observations revealed the presence of one of the largest masses of cold dust (greater than 0.2 M ) ever measured in a SNR.…”

Section: Supernova Remnants In the Magellanic Cloudsmentioning

confidence: 81%

Radio Emission from Supernova Remnants

Dubner

2016

Handbook of Supernovae

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The explosion of a supernova releases almost instantaneously about 10 51 ergs of mechanic energy, changing irreversibly the physical and chemical properties of large regions in the galaxies. The stellar ejecta, the nebula resulting from the powerful shock waves, and sometimes a compact stellar remnant, constitute a supernova remnant (SNR). They can radiate their energy across the whole electromagnetic spectrum, but the great majority are radio sources. Almost 70 years after the first detection of radio emission coming from a SNR, great progress has been achieved in the comprehension of their physical characteristics and evolution. We review the present knowledge of different aspects of radio remnants, focusing on sources of the Milky Way and the Magellanic Clouds, where the SNRs can be spatially resolved. We present a brief overview of theoretical background, analyze morphology and polarization properties, and review and critical discuss different methods applied to determine the radio spectrum and distances. The consequences of the interaction between the SNR shocks and the surrounding medium are examined, including the question of whether SNRs can trigger the formation of new stars. Cases of multispectral comparison are presented. A section is devoted to reviewing recent results of radio SNRs in the Magellanic Clouds, with particular emphasis on the radio properties of SN 1987A, an ideal laboratory to investigate dynamical evolution of an SNR in near real time. The review concludes with a summary of issues on radio SNRs that deserve fur-G. Dubner and E. Giacani are members of the "Carrera del Investigador Científico" of CONICET, Argentina

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

Cited by 20 publications

References 21 publications

High Angular Resolution ALMA Images of Dust and Molecules in the SN 1987A Ejecta

High Angular Resolution ALMA Images of Dust and Molecules in the SN 1987A Ejecta

Late Spectral Evolution of the Ejecta and Reverse Shock in Sn 1987a

Radio Emission from Supernova Remnants

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