Cassiopeia A: dust factory revealed via submillimetre polarimetry

Dunne, L.; Maddox, S.; Ivison, R. J.; Rudnick, Lawrence; DeLaney, Tracey; Matthews, Brenda C.; Crowe, C. M.; Gomez, Haley Louise; Eales, Stephen Anthony; Dye, S.

doi:10.1111/j.1365-2966.2009.14453.x

Cited by 96 publications

(141 citation statements)

References 62 publications

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“…The "maximum" SN efficiency originates from theoretical SN dust formation models, and corresponds to dust masses of approximately 3-10 × 10 −1 M . Similar dust masses have been observed in SN remnants such as Cas A (e.g., Dunne et al 2009) or Kepler (e.g., Gomez et al 2009). Dust destruction in reverse shock interaction of about 93% has been applied to the "maximum" SN efficiency, to obtain the "high" SN efficiency.…”

Section: The Modelsupporting

confidence: 77%

“…There is only little observational evidence that SNe can be very efficient (e.g., Wilson & Batrla 2005;Douvion et al 2001;Dunne et al 2009), and theoretical models predict significant dust destruction in reverse shocks of SNe (e.g., Bianchi & Schneider 2007;Nozawa et al 2007Nozawa et al , 2010. On the other hand, these models also show that the effectiveness of dust destruction depends on various properties such as the geometry of the shocks, the density of the ejecta and the ISM, the size and shape of the grains, clumping in the SNe ejecta, and different SN types.…”

Section: Sn Efficiency and Mass Of The Galaxymentioning

confidence: 99%

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Genesis and evolution of dust in galaxies in the early Universe

Gall

Andersen

Hjorth

2011

A&A

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Aims. We intend to assess the most plausible scenarios for generating large amounts of dust in high-z quasars (QSOs) on the basis of observationally derived physical properties of QSOs at z 6. Methods. We use a chemical evolution model to compute the temporal progression of quantities such as the amount of dust and gas, stellar masses, star formation rates (SFRs) and the metallicity for various combinations of the initial mass function (IMF), the mass of the galaxy, dust production efficiencies, and the degree of dust destruction in the ISM. We investigate the influence of the SFR on the evolution of these quantities, and determine the earliest epochs at which agreement with observations can be achieved. We apply the obtained results to individual QSOs at z 6. Results. We find that large quantities of dust can be generated rapidly as early as 30 Myr after the onset of the starburst when the SFR of the starburst is 10 3 M yr −1 . The amount of dust and several other physical quantities of individual QSOs at z 6 are satisfactorily reproduced by models at epochs 30, 70, 100, and 170 Myr for galaxies with initial gas masses of 1-3 × 10 11 M . The best agreement with observations is obtained with top-heavy IMFs. A sizable dust contribution from supernovae (SNe) is however required, while at these epochs dust production by asymptotic giant branch (AGB) stars is negligible. Moderate dust destruction in the ISM can be accommodated.

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Section: The Modelsupporting

confidence: 77%

Section: Sn Efficiency and Mass Of The Galaxymentioning

confidence: 99%

Genesis and evolution of dust in galaxies in the early Universe

Gall

Andersen

Hjorth

2011

A&A

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“…This implies that a typical 20 M star now produces nearly 0.08 M of dust. This is 2-3 times higher than the maximum amount of warm dust observed in SNII (Rho et al 2008(Rho et al , 2009), yet lower than the most recent estimates of the cold dust mass in the Kepler and CasA SN remnants (Gomez et al 2009;Dunne et al 2009). The dust "yields" as a function of stellar mass for SNeII are shown in Fig.…”

Section: Dust Productionmentioning

confidence: 54%

“…In fact, while submillimetre observations of the Kepler and CasA SN remnants yield 0.1-1 M of dust (e.g. Morgan et al 2003;Dunne et al 2009;Gomez et al 2009), infrared observations give 0.1 M of dust (Helmhamdi et al 2003;Sugerman et al 2006;Kotak et al 2009;Rho et al 2008Rho et al , 2009Meikle et al 2007;Takaya et al 2008). A possibility is that such a discrepancy could be traced back to a difference in the instrument sensitivity to the different dust phases (cold for submillimetre, warm for Spitzer).…”

Section: Introductionmentioning

confidence: 99%

The chemical evolution of elliptical galaxies with stellar and QSO dust production

Pipino

Fan

Matteuccí

et al. 2010

A&A

145

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Context. The presence of dust strongly affects the way we see galaxies and also the chemical abundances we measure in gas. It is therefore important to study the chemical evolution of galaxies by taking into account dust evolution. Aims. We aim at performing a detailed study of abundance ratios of high redshift objects and their dust properties. We focus on Lyman-Break galaxies (LBGs) and Quasar (QSO) hosts as likely progenitors of low-and high-mass present-day elliptical galaxies, respectively. Methods. We have adopted a chemical evolution model for elliptical galaxies taking into account the dust production from low and intermediate mass stars, supernovae Ia, supernovae II, QSOs and both dust destruction and accretion processes. By means of such a model we have followed the chemical evolution of ellipticals of different baryonic masses. Our model complies with chemical downsizing.Results. We made predictions for the abundance ratios versus metallicity trends for models of differing masses that can be used to constrain the star formation rate, initial mass function and dust mass in observed galaxies. We predict the existence of a high redshift dust mass-stellar mass relationship. We have found a good agreement with the properties of LBGs if we assume that they formed at redshift z = 2-4. In particular, a non-negligible amount of dust is needed to explain the observed abundance pattern. We studied the QSO SDSS J114816, one of the most distant QSO ever observed (z = 6.4), and we have been able to reproduce the amount of dust measured in this object. The dust is clearly due to the production from supernovae and the most massive AGB stars as well as from the grain growth in the interstellar medium. The QSO dust is likely to dominate only in the very central regions of the galaxies and during the early development of the galactic wind.

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“…The underlying dust formation models are sensitive to assumptions about the parameters controlling the dust grain properties (such as morphology, size, or composition; Gall et al 2011c;Fallest et al 2011) which determine the shape and characteristics of extinction curves (see Section 6.5). Furthermore, dust grains produced by SNe will be subject to either disruptive, destructive, or growth processes due to, for example, shock interactions in the SN remnant (e.g., Bianchi & Schneider 2007;Nozawa et al 2007;Dunne et al 2009;Matsuura et al 2011) or the interstellar medium (e.g., Draine 2009;Michałowski et al 2010a), or due to reprocessing by the intense UV radiation in star-forming regions. Any modifications of the original dust grains formed by SNe will lead to changes in either the mineralogy or the grainsize distribution of the dust, and hence the resulting extinction law (e.g., Hirashita & Kuo 2011).…”

Section: Introductionmentioning

confidence: 99%

ON INFERRING EXTINCTION LAWS INz∼ 6 QUASARS AS SIGNATURES OF SUPERNOVA DUST

Hjorth

Vreeswijk

Gall

et al. 2013

ApJ

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Unusual extinction curves of high-redshift QSOs have been taken as evidence that dust is primarily produced by supernovae at high redshift. In particular, the 3000 Å Todini-Ferrara-Maiolino kink in the extinction curve of the z = 6.20 SDSS J1048+4637 has been attributed to supernova dust. Here we discuss the challenges in inferring robust extinction curves of high-redshift QSOs and critically assess previous claims of detection of supernova dust. In particular, we address the sensitivity to the choice of intrinsic QSO spectrum, the need for a long wavelength baseline, and the drawbacks in fitting theoretical extinction curves. In a sample of 21 QSOs at z ∼ 6 we detect significant ultraviolet extinction using existing broadband optical, near-infrared, and Spitzer photometry. The median extinction curve is consistent with a Small Magellanic Cloud curve with A 1450 ∼ 0.7 mag and does not exhibit any conspicuous (rest frame) 2175 Å or 3000 Å features. For two QSOs, SDSS J1044−0125 at z = 5.78 and SDSS J1030+0524 at z = 6.31, we further present X-shooter spectra covering the wavelength range 0.9-2.5 μm. The resulting non-parametric extinction curves do not exhibit the 3000 Å kink. Finally, in a re-analysis of literature spectra of SDSS J1048+4637, we do not find evidence for a conspicuous kink. We conclude that the existing evidence for a 3000 Å feature is weak and that the overall dust properties at high and low redshifts show no significant differences. This, however, does not preclude supernovae from dominating the dust budget at high redshift.

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Cassiopeia A: dust factory revealed via submillimetre polarimetry

Cited by 96 publications

References 62 publications

Genesis and evolution of dust in galaxies in the early Universe

Genesis and evolution of dust in galaxies in the early Universe

The chemical evolution of elliptical galaxies with stellar and QSO dust production

ON INFERRING EXTINCTION LAWS INz∼ 6 QUASARS AS SIGNATURES OF SUPERNOVA DUST

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