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Type Ia Supernova Host Galaxies As Seen with IFU Spectroscopy? Stanishev, V.1, Rodrigues, M.2,3, Mourao,˜ A.1, and Flores, H.2

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Type Ia Supernova Host Galaxies As Seen with IFU Spectroscopy? Stanishev, V.1, Rodrigues, M.2,3, Mourao,˜ A.1, and Flores, H.2 Astronomy & Astrophysics manuscript no. ms˙edited c ESO 2021 September 1, 2021 Type Ia Supernova host galaxies as seen with IFU spectroscopy? Stanishev, V.1, Rodrigues, M.2;3, Mourao,˜ A.1, and Flores, H.2 1 CENTRA - Centro Multidisciplinar de Astrof´ısica, Instituto Superior Tecnico,´ Av. Rovisco Pais 1, 1049-001 Lisbon, Portugal 2 GEPI , Observatoire de Paris, CNRS, University Paris Diderot, 5 Place Jules Janssen, 92195 Meudon, France 3 European Southern Observatory, Alonso de Cordova 3107, Casilla 19001, Vitacura, Santiago, Chile Received data Accepted date ABSTRACT Context. Type Ia Supernovae (SNe Ia) have been widely used in cosmology as distance indicators. However, to fully exploit their potential in cosmology, a better control over systematic uncertainties is required. Some of the uncertainties are related to the unknown nature of the SN Ia progenitors. Aims. We aim to test the use of integral field unit (IFU) spectroscopy for correlating the properties of nearby SNe Ia with the properties of their host galaxies at the location of the SNe. The results are to be compared with those obtained from an analysis of the total host spectrum. The goal is to explore this path of constraining the nature of the SN Ia progenitors and further improve the use of SNe Ia in cosmology. Methods. We used the wide-field IFU spectrograph PMAS/PPAK at the 3.5m telescope of Calar Alto Observatory to observe six nearby spiral galaxies that hosted SNe Ia. Spatially resolved 2D maps of the properties of the ionized gas and the stellar populations were derived. −1 Results. Five of the observed galaxies have an ongoing star formation rate of 1-5 M yr and mean stellar population ages ∼ 5 Gyr. The sixth galaxy shows no star formation and has an about 12 Gyr old stellar population. All galaxies have stellar masses larger than 10 2 × 10 M and metallicities above solar. Four galaxies show negative radial metallicity gradients of the ionized gas up to −0:058 dex kpc−1 and one has nearly uniform metallicity with a possible shallow positive slope. The stellar components show shallower negative metallicity gradients up to −0:03 dex kpc−1. We find no clear correlation between the properties of the galaxy and those of the supernovae, which may be because of the small ranges spanned by the galaxy parameters. However, we note that the Hubble residuals are on average positive while negative Hubble residuals are expected for SNe Ia in massive hosts such as the galaxies in our sample. Conclusions. The IFU spectroscopy on 4-m telescopes is a viable technique for studying host galaxies of nearby SNe Ia. It allows one to correlate the supernova properties with the properties of their host galaxies at the projected positions of the supernovae. Our current sample of six galaxies is too small to draw conclusions about the SN Ia progenitors or correlations with the galaxy properties, but the ongoing CALIFA IFU survey will provide a solid basis to exploit this technique more and improve our understanding of SNe Ia as cosmological standard candles. Key words. Galaxies: general – Galaxies: abundances – (Stars:) supernovae: general 1. Introduction reduced to a level below ∼ 2% to differentiate between different dark energy models. More than a decade ago the observations of Type Ia Supernovae (SNe Ia) led to the discovery of the accelerating expansion of the The use of SNe Ia in Cosmology relies on the empirically Universe and the need for an unknown repulsive force to drive it established tight relation between their light curve width and (Perlmutter et al. 1999; Riess et al. 1998). Understanding the na- peak luminosity, which allows one to measure the luminosity ∼ ture of this force – now dubbed ”dark energy” – is an outstanding distance with an accuracy of 7% (Phillips et al. 1999), and on goal of astrophysics and cosmology. It is now well-understood the assumption that the (standardized) peak luminosity of SNe that no single observational technique will be able to achieve this Ia does not change over the cosmic time. There is now obser- alone (e.g. Albrecht et al. 2006). The combined constraints of vational evidence that the slope of the ”light curve shape - peak many techniques will be needed to measure the equation-of-state luminosity” relation does not depend on the redshift or the host arXiv:1205.5183v3 [astro-ph.CO] 30 May 2012 parameter of the dark energy (the ratio between the pressure and galaxy mass (Conley et al. 2011; Sullivan et al. 2011). However, the density) and eventually its evolution over the cosmic time. At Sullivan et al. (2010) and Kelly et al. (2010) have found that the present, SNe Ia is the most matured and well-understood tech- offsets of the SN Ia peak magnitudes from the best-fitting Hubble nique to accurately trace the cosmic expansion history and will line (from now on Hubble residuals or HR) correlate with the continue to play an essential role in future cosmological experi- host stellar mass. Together with the mass-metallicity relation for ments (Albrecht et al. 2006). However, the SNe Ia technique is galaxies (e.g., Tremonti et al. 2004) and the overall increase of affected by several systematic uncertainties, which need to be the metal content of the universe with the cosmic time, this may be an indication for possible luminosity evolution of SNe Ia at a level of 0.05-0.10 mag. ? Based on observations collected at the Centro Astronomico´ Hispano Aleman´ (CAHA) at Calar Alto, operated jointly by the Max- It is now generally agreed that SNe Ia are the result Planck Institut fur¨ Astronomie and the Instituto de Astrof´ısica de of thermonuclear disruption of carbon/oxygen (C/O) white Andaluc´ıa (CSIC) dwarfs (WD), which ignite explosively when they approach the 1 Stanishev, V. et al.: Type Ia Supernova host galaxies as seen with IFU spectroscopy Chandrasekhar limit MCh ∼ 1:38M (Hoyle & Fowler 1960). itor star of an SN Ia (Bloom et al. 2012; Chomiuk et al. 2012; However, there has been little observational evidence of the Nugent et al. 2011). The results reinforce the conclusion that the exact evolutionary scenario that leads to the explosion. C/O exploding star is a C/O WD and seem to rule out all but a de- WDs are the end product of the evolution of stars with masses generate star as its companion, thus favoring the DD scenario. ∼ 1:5 − 7M (e.g., see Becker & Iben 1980; Dom´ınguez et al. On the other hand, based on high-resolution spectroscopy of a 1999). The upper mass limit for C/O WDs is ∼ 1:1M (e.g., see sample of nearby SNe Ia Sternberg et al. (2011) favor the SD Dom´ınguez et al. 1999; Salaris et al. 2009; Weidemann 1987) scenario. and therefore a mechanism that allows the WD to gain addi- Many studies have shown that the intrinsically luminous SNe tional mass of at least ∼ 0:3 − 0:4M is needed. In the single tend to occur in star-forming hosts, while the faint SNe pre- degenerate (SD) scenario the WD accretes mass from a non- fer passive ones (e.g., Brandt et al. 2010; Gallagher et al. 2005, degenerate companion star in a binary system (Whelan & Iben 2008; Hamuy et al. 1996, 2000; Howell et al. 2009; Kelly et al. 1973). However, the exact physical mechanism of the WD mass 2010; Neill et al. 2009; Raskin et al. 2009; Sullivan et al. 2010, growth has not yet been identified. In the double-degenerate 2006). Gallagher et al. (2008) found that the Hubble residuals (DD) scenario two C/O WDs in a binary merge after loosing or- correlate with the global host metallicity. Sullivan et al. (2010) bital angular momentum by gravitational wave radiation (Iben & and Kelly et al. (2010) found such a correlation with the host Tutukov 1984; Paczynski 1985; Webbink 1984). While consid- stellar mass. However, Howell et al. (2009), who used the galaxy ered the most viable, both scenarios have considerable uncertain- stellar mass as a proxy for the metallicity, found no such correla- ties (see, e.g. Hillebrandt & Niemeyer 2000; Maoz & Mannucci tion and suggested that instead the progenitor age may be a more 2011). important parameter. The numerical simulations of thermonuclear SN Ia explo- All studies of SN Ia hosts galaxies conducted so far, except sions suggest that the properties of the exploding WD may sig- that by Raskin et al. (2009), were based on an analysis of the nificantly influence the peak luminosity, the ”light curve width - global photometric or spectroscopic properties of the host galax- luminosity” relation and colors of the resulting supernovae (e.g., ies. In this paper we take a different approach. We use for the Bravo et al. 2010; Dom´ınguez et al. 2001; Hoflich¨ et al. 1998; first time integral field unit (IFU) spectroscopy at intermediate Kasen et al. 2009; Ropke¨ et al. 2006; Umeda et al. 1999). On spectral resolution to study a sample of host galaxies of local the other hand, the properties of the WD just before the ignition SNe Ia (z ∼ 0:02). This approach has an advantage over the pre- (the central density, metallicity and C/O ratio) are sensitive to the vious studies because it allows us to derive spatially-resolved properties and the evolution of its progenitor binary star, and to two-dimensional (2D) maps of host galaxy properties, e.g. the the subsequent WD mass growth mechanism. For example, the heavy element abundance in the interstellar medium (ISM). The SD channel can produce MCh WDs with slightly different struc- intermediate spectral resolution makes it also possible to use ture and chemical composition depending on the mass of the full-spectrum fitting techniques to derive 2D maps of the prop- WD at the moment when the accretion started (e.g., Dom´ınguez erties of the stellar populations.
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