Dust extinction towards the type Ia supernova 2012cu in NGC 4772

Gao, Weijia; Zhao, Ruining; Jian, Gao; Jiang, Biwei; Li, J.

doi:10.1016/j.pss.2018.12.010

Cited by 10 publications

(10 citation statements)

References 53 publications

(82 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Therefore, it suggests that a single parameter of 𝑅 𝑉 is insufficient to completely represent the extinction curve of SN 2010jl and the detailed dust properties around SN 2010jl. The empirical single parameter extinction curves of CCM89 or F99 is not suitable and sufficient to explain the extinction curves of Type IIn supernovae or the extinction laws outside the MW (Gao et al 2015;Li & Draine 2001;Gao et al 2020). From the results in Table 4, there is no obvious time-dependent variation of 𝑅 𝑉 after 100 days for the dust around SN 2010jl.…”

Section: The Extinction Law Of Sn 2010jlmentioning

confidence: 92%

Dust Models for the Extinction of Type IIn Supernova SN 2010jl

Li,

Gao,

Jiang

et al. 2022

Preprint

Self Cite

View full text Add to dashboard Cite

The unusual extinction curves of SN 2010jl provide an excellent opportunity to investigate the properties of dust formed by core-collapse supernovae. By using a series of dust models with different compositions and grain size distributions, we fit the extinction curves of SN 2010jl and find that a silicate-graphite mixture dust model characterized by exponentially cutoff powerlaw size distributions can well reproduce its unusual extinction curves. The best-fit results show that the extinctions derived from the dust models are consistent with the observed values at all epochs. However, the total-to-selective extinction ratio 𝑅 𝑉 is about 2.8 -3.1, which is significantly smaller than the value of 𝑅 𝑉 ≈ 6.4 derived by Gall et al. The best-fit models indicate that the dust grains around SN 2010jl are possibly composed of small-size astronomical silicate grains and micron-size graphite grains. In addition, by fitting the optical to mid-infrared spectral energy distribution, we find that the dust mass around SN 2010jl increases with time, up to 0.005 𝑀 around 1300 days after peak brightness, which is consistent with previous estimates.

show abstract

Section: The Extinction Law Of Sn 2010jlmentioning

confidence: 92%

Dust Models for the Extinction of Type IIn Supernova SN 2010jl

Li,

Gao,

Jiang

et al. 2022

Preprint

Self Cite

View full text Add to dashboard Cite

show abstract

“…The shape of the curve given in Equation 2 is consistent with the results in Nozawa et al (2015), with r 0 = 0.05 µm representing small size of dust grains with average radius of 0.045 µm. The size of dust grains on the line-of-sight to SNe Ia is likely to be smaller than typical dust grains in the Milky Way, as may be inferred from the low values of total-to-selective extinction ratio for typical SNe Ia (Wang 2005;Wang et al 2006;Foley et al 2014;Amanullah et al 2015;Gao et al 2020). In addition, only silicate grains with single chemical composition are considered in our models, the difference is insignificant for models with both silicate and graphite grains (Gao et al 2015).…”

Section: Dust Propertiesmentioning

confidence: 99%

The Effects of Circumstellar Dust Scattering on the Light Curves and Polarizations of Type Ia Supernovae

Hu,

Wang,

Wang

2021

Preprint

View full text Add to dashboard Cite

Observational signatures of the circumstellar material (CSM) around Type Ia supernovae (SNe Ia) provide a unique perspective to the progenitor systems. The pre-supernova evolution of the SN progenitors may naturally eject CSM in most of the popular scenarios of SN Ia explosions. In this study, we investigate the influence of dust scattering on the light curves and polarizations of SNe Ia. A Monte Carlo method is constructed to numerically solve the radiative transfer process through the CSM. Three types of geometric distributions of the CSM are considered: spherical shell, axisymmetric disk, and axisymmetric shell. We show that both the distance of the dust to the SNe and the geometric distribution of the dust affect the light curve and color evolutions of SNe. Contrary to previous studies, we found that the geometric location of the hypothetical CS dust cannot be reliably constrained based on photometric data alone even for the best observed cases such as SN 2006X and SN 2014J, and time dependent polarimetry is an inimitable way to establish the geometric location of any dusty CSM. Our model results show that time sequence of broad-band polarimetry with appropriate time coverage from a months to about one year after explosion can provide unambiguous limits on the presence of CS dust around SNe Ia.

show abstract

“…The interstellar abundances in M31 can thus be assumed to be similar to those in the MW with protosolar values (Asplund et al 2009). We consider the mass ratio of graphite to silicate to be f cs = 0.3 as a typical value used in previous works (Gao et al 2013;Wang et al 2014;Gao et al 2015Gao et al , 2020) and adopted in Draine et al (2014), which means that the elements of Fe, Mg and Si are all in the solid phase and constrained in silicate dust, and that the fraction of gas-phase carbon is 50%.…”

Section: Dust Extinction Modelmentioning

confidence: 99%

“…In addition, although they have similar R V values, the extinction curve of the SMC bar (R V ≈ 2.74) varies substantially from that of the SMC wing (R V ≈ 2.05) (see Figure 1 and Figure 6). Therefore, R V cannot generally be applied to external galaxies such as SMC (Lequeux et al 1982;Prevot et al 1984;Gordon et al 2003), starburst galaxies (Calzetti et al 1994;Calzetti 2001Calzetti , 1997Calzetti et al 2000), type Ia supernova (Gao et al 2015(Gao et al , 2020, etc.…”

Section: Thementioning

confidence: 99%

“…This second UV bump is due to the sharp absorption edge of the "astronomical silicate" dielectric function inDraine & Lee (1984) based on laboratory measurements of crystalline olivine (Mg, Fe) 2 SiO 4 inHuffman & Stapp (1973). The dielectric function for "astronomical silicate" inDraine & Lee (1984) is typical and is the basis for modeling extinction laws with the silicate-graphite dust model(Weingartner & Draine 2001;Li & Draine 2001;Wang et al 2014;Gao et al 2015Gao et al , 2020.…”

mentioning

confidence: 99%

See 1 more Smart Citation

Dust Extinction Law in Nearby Star-Resolved Galaxies. I. M31 Traced by Supergiants

Wang,

Gao,

Ren

2021

Preprint

Self Cite

View full text Add to dashboard Cite

The dust extinction laws and dust properties in M31 are explored with a sample of reddened O-type and B-type supergiants obtained from the LGGS. The observed spectral energy distributions (SEDs) for each tracer are constructed with multiband photometry from the LGGS, PS1 Survey, UKIRT, PHAT Survey, Swift/UVOT and XMM-SUSS. We model the SED for each tracer in combination with the intrinsic spectrum obtained from the stellar model atmosphere extinguished by the model extinction curves. Instead of mathematically parameterizing the extinction functions, the model extinction curves in this work are directly derived from the silicate-graphite dust model with a dust size distribution of dn/da ∼ a −α exp(−a/0.25), 0.005 < a < 5 µm. The extinction tracers are distributed along the arms in M31, with the derived MW-type extinction curves covering a wide range of R V (≈ 2 − 6), indicating the complexity of the interstellar en-

show abstract

Dust extinction towards the type Ia supernova 2012cu in NGC 4772

Cited by 10 publications

References 53 publications

Dust Models for the Extinction of Type IIn Supernova SN 2010jl

Dust Models for the Extinction of Type IIn Supernova SN 2010jl

The Effects of Circumstellar Dust Scattering on the Light Curves and Polarizations of Type Ia Supernovae

Dust Extinction Law in Nearby Star-Resolved Galaxies. I. M31 Traced by Supergiants

Contact Info

Product

Resources

About