scholarly journals The dependence of Type Ia Supernovae salt2 light-curve parameters on host galaxy morphology

2020 ◽  
Vol 499 (4) ◽  
pp. 5121-5135
Author(s):  
M V Pruzhinskaya ◽  
A K Novinskaya ◽  
N Pauna ◽  
P Rosnet
Keyword(s):  
Light Curve ◽  
Host Galaxy ◽  
Type Ia Supernovae ◽  
Distance Modulus ◽  
Early Type ◽  
Late Type ◽  
Hubble Diagram ◽  
Type Ia ◽  
Ia Supernovae ◽  
Galaxy Morphology

ABSTRACT Type Ia Supernovae (SNe Ia) are widely used to measure distances in the Universe. Despite the recent progress achieved in SN Ia standardization, the Hubble diagram still shows some remaining intrinsic dispersion. The remaining scatter in supernova luminosity could be due to the environmental effects that are accounted for as mass step correction in the current cosmological analyses. In this work, we compare the local and global colour (U − V), the local star formation rate, and the host stellar mass to the host galaxy morphology. The observed trends suggest that the host galaxy morphology is a relevant parameter to characterize the SN Ia environment. Therefore, we study the influence of host galaxy morphology on light-curve parameters of SNe Ia from the pantheon cosmological supernova sample. We determine the Hubble morphological type of host galaxies for a subsample of 330 SNe Ia. We confirm that the salt2 stretch parameter x1 depends on the host morphology with the p-value ∼10−14. The supernovae with lower stretch value are hosted mainly by elliptical and lenticular galaxies. No correlation for the salt2 colour parameter c is found. We also examine Hubble diagram residuals for supernovae hosted by ‘early-type’ and ‘late-type’ morphological groups of galaxies. The analysis reveals that the mean distance modulus residual in early-type galaxies is smaller than the one in late-type galaxies, which means that early-type galaxies contain brighter supernovae after stretch and colour corrections. However, we do not observe any difference in the residual dispersion for these two morphological groups. The obtained results are in the line with other analyses showing environmental dependence of SN Ia light-curve parameters and luminosity. We confirm the importance of including a host galaxy parameter into the standardization procedure of SNe Ia for further cosmological studies.

scholarly journals The Hubble diagram of type Ia supernovae as a function of host galaxy morphology

2003 ◽  
Vol 340 (4) ◽  
pp. 1057-1075 ◽  
Author(s):  
M. Sullivan ◽  
R. S. Ellis ◽  
G. Aldering ◽  
R. Amanullah ◽  
P. Astier ◽  
...  
Keyword(s):  
Host Galaxy ◽  
Type Ia Supernovae ◽  
Hubble Diagram ◽  
Type Ia ◽  
Ia Supernovae ◽  
Galaxy Morphology

scholarly journals The Host Galaxies of High-Redshift Type Ia Supernovae

2005 ◽  
Vol 192 ◽  
pp. 555-560
Author(s):  
Mark Sullivan ◽  
Richard Ellis ◽  
Keyword(s):  
Cosmological Constant ◽  
High Redshift ◽  
Cosmological Parameters ◽  
Type Systems ◽  
Host Galaxy ◽  
Type Ia Supernovae ◽  
Early Type ◽  
Late Type ◽  
Type Ia ◽  
Ia Supernovae

SummaryWe present new results on the Hubble diagram of distant type Ia supernovae (SNe Ia) segregated according to the type of host galaxy. This makes it possible to check earlier evidence for a cosmological constant by explicitly comparing SNe residing in galaxies likely to contain negligible dust with the larger sample. The cosmological parameters derived from these SNe Ia hosted by presumed dust-free early-type galaxies support earlier claims for a cosmological constant, which we demonstrate at ≃ 5σ significance, and the internal extinction implied is small even for late-type systems (AB < 0.2). Furthermore, the scatter observed in the SNe Ia Hubble diagrams correlates closely with host galaxy morphology. We find this scatter is smallest for SNe Ia occurring in early-type hosts and largest for those in late-type galaxies. Moreover, SNe residing in late-type hosts appear fainter in their light-curve-width-corrected luminosity than those in early-type hosts, as expected if a modest amount of dust extinction is a contributing factor. Thus, our data demonstrate that host galaxy extinction is unlikely to systematically dim distant SNe Ia in a manner that would produce a spurious cosmological constant.

scholarly journals Observations of Type Ia Supernovae and Challenges for Cosmology

2005 ◽  
Vol 192 ◽  
pp. 525-533
Author(s):  
Weidong Li ◽  
Alexei V. Filippenko
Keyword(s):  
Dark Energy ◽  
Light Curve ◽  
Rise Time ◽  
Accelerating Universe ◽  
Type Ia Supernovae ◽  
Hubble Diagram ◽  
High Quality ◽  
Type Ia ◽  
Secondary Parameter ◽  
Ia Supernovae

SummaryObservations of Type Ia supernovae (SNe Ia) reveal correlations between their luminosities and light-curve shapes, and between their spectral sequence and photometric sequence. Assuming SNe Ia do not evolve at different redshifts, the Hubble diagram of SNe Ia may indicate an accelerating Universe, the signature of a cosmological constant or other forms of dark energy. Several studies raise concerns about the evolution of SNe Ia (e.g., the peculiarity rate, the rise time, and the color of SNe Ia at different redshifts), but all these studies suffer from the difficulties of obtaining high-quality spectroscopy and photometry for SNe Ia at high redshifts. There are also some troubling cases of SNe Ia that provide counter examples to the observed correlations, suggesting that a secondary parameter is necessary to describe the whole SN Ia family. Understanding SNe Ia both observationally and theoretically will be the key to boosting confidence in the SN Ia cosmological results.

On the progenitors of type IA supernovae in early-type and late-type galaxies

1994 ◽  
Vol 423 ◽  
pp. L31 ◽  
Author(s):  
Massimo della Valle ◽  
Mario Livio
Keyword(s):  
Type Ia Supernovae ◽  
Early Type ◽  
Late Type ◽  
Type Ia ◽  
Ia Supernovae

scholarly journals Influence of host galaxy morphology on the properties of Type Ia supernovae from JLA and Pantheon compilations

2020 ◽  
Author(s):  
Maria Pruzhinskaya ◽  
Alexandra Novinskaya ◽  
Philippe Rosnet ◽  
Nicoleta Pauna
Keyword(s):  
Host Galaxy ◽  
Type Ia Supernovae ◽  
Type Ia ◽  
Ia Supernovae ◽  
Galaxy Morphology

scholarly journals Light Curve Models for SN 2009dc

2011 ◽  
Vol 7 (S281) ◽  
pp. 314-315
Author(s):  
Yasuomi Kamiya
Keyword(s):  
Light Curve ◽  
White Dwarfs ◽  
Light Curves ◽  
Host Galaxy ◽  
Type Ia Supernovae ◽  
Radiation Hydrodynamics ◽  
One Dimensional ◽  
Type Ia ◽  
Ia Supernovae

AbstractSimplified explosion models of super-Chandrasekhar-mass C-O white dwarfs (WDs) are constructed with parameters such as WD mass and 56Ni mass. Their light curves are obtained by solving one-dimensional equations of radiation hydrodynamics, and compared with the observations of SN 2009dc, one of the overluminous Type Ia supernovae, to estimate its properties. As a result, the progenitor of SN 2009dc is suggested to be a 2.2–2.4-M⊙ C-O WD with 1.2–1.4 M⊙ of 56Ni, if the extinction by its host galaxy is negligible.

scholarly journals The influence of host galaxy morphology on the properties of Type Ia supernovae from the JLA compilation

New Astronomy ◽  
2017 ◽  
Vol 51 ◽  
pp. 43-50 ◽  
Author(s):  
V. Henne ◽  
M.V. Pruzhinskaya ◽  
P. Rosnet ◽  
P.-F. Léget ◽  
E.E.O. Ishida ◽  
...  
Keyword(s):  
Host Galaxy ◽  
Type Ia Supernovae ◽  
Type Ia ◽  
Ia Supernovae ◽  
Galaxy Morphology

scholarly journals Constraints on the density distribution of type Ia supernovae ejecta inferred from late-time light-curve flattening

2020 ◽  
Vol 493 (4) ◽  
pp. 5617-5624
Author(s):  
Doron Kushnir ◽  
Eli Waxman
Keyword(s):  
Light Curve ◽  
Weighted Average ◽  
Far Infrared ◽  
Average Density ◽  
Light Curves ◽  
Type Ia Supernovae ◽  
Late Time ◽  
Simple Method ◽  
Type Ia ◽  
Ia Supernovae

ABSTRACT The finite time, τdep, over which positrons from β+ decays of 56Co deposit energy in type Ia supernovae ejecta lead, in case the positrons are trapped, to a slower decay of the bolometric luminosity compared to an exponential decline. Significant light-curve flattening is obtained when the ejecta density drops below the value for which τdep equals the 56Co lifetime. We provide a simple method to accurately describe this ‘delayed deposition’ effect, which is straightforward to use for analysis of observed light curves. We find that the ejecta heating is dominated by delayed deposition typically from 600 to 1200 d, and only later by longer lived isotopes 57Co and 55Fe decay (assuming solar abundance). For the relatively narrow 56Ni velocity distributions of commonly studied explosion models, the modification of the light curve depends mainly on the 56Ni mass-weighted average density, 〈ρ〉t3. Accurate late-time bolometric light curves, which may be obtained with JWST far-infrared (far-IR) measurements, will thus enable to discriminate between explosion models by determining 〈ρ〉t3 (and the 57Co and 55Fe abundances). The flattening of light curves inferred from recent observations, which is uncertain due to the lack of far-IR data, is readily explained by delayed deposition in models with $\langle \rho \rangle t^{3} \approx 0.2\, \mathrm{M}_{\odot }\, (10^{4}\, \textrm{km}\, \textrm{s}^{-1})^{-3}$, and does not imply supersolar 57Co and 55Fe abundances.

scholarly journals Star formation in early-type galaxies: the role of stellar winds and kinematics

2015 ◽  
Vol 11 (S315) ◽  
Author(s):  
Silvia Pellegrini ◽  
Andrea Negri ◽  
Luca Ciotti
Keyword(s):  
Star Formation ◽  
High Resolution ◽  
Type Ia Supernovae ◽  
Stellar Winds ◽  
Early Type ◽  
Stellar Component ◽  
Type Ia ◽  
Hydrodynamical Simulations ◽  
Ia Supernovae

AbstractEarly-type galaxies (ETGs) host a hot ISM produced mainly by stellar winds, and heated by Type Ia supernovae and the thermalization of stellar motions. High resolution 2D hydrodynamical simulations showed that ordered rotation in the stellar component results in the formation of a centrifugally supported cold equatorial disc. In a recent numerical investigation we found that subsequent generations of stars are formed in this cold disc; this process consumes most of the cold gas, leaving at the present epoch cold masses comparable to those observed. Most of the new stellar mass formed a few Gyrs ago, and resides in a disc.

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