Early-type galaxies with core collapse supernovae

Hakobyan, A. A.; Петросян, А. Р.; McLean, B.; Kunth, D.; Allen, R. J.; Turatto, M.; Barbon, R.

doi:10.1051/0004-6361:200809817

Cited by 51 publications

(57 citation statements)

References 79 publications

(107 reference statements)

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“…Such a location of SN is in good agreement with the known correlations of core-collapse (Types Ibc and II) SNe with star formation in galaxies (e.g. James & Anderson 2006;Hakobyan et al 2008), including also star formation induced by an interaction with neighbor galaxies (e.g. Nazaryan et al 2013;Hakobyan et al 2014).…”

Section: Description Of the Systemsupporting

confidence: 88%

Hα Velocity Fields and Galaxy Interaction in the Quartet of Galaxies NGC 7769, 7770, 7771 and 7771A

2016

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Abstract. The quartet of galaxies NGC 7769, 7770, 7771 and 7771A is a system of interacting galaxies. Close interaction between galaxies caused characteristic morphological features: tidal arms and bars, as well as an induced star formation. In this study, we performed the Fabry-Perot scanning interferometry of the system in Hα line and studied the velocity fields of the galaxies. We found that the rotation curve of NGC 7769 is weakly distorted. The rotation curve of NGC 7771 is strongly distorted with the tidal arms caused by direct flyby of NGC 7769 and flyby of a smaller neighbor NGC 7770. The rotation curve of NGC 7770 is significantly skewed because of the interaction with the much massive NGC 7771. The rotation curves and morphological disturbances suggest that the NGC 7769 and NGC 7771 have passed the first pericenter stage, however, probably the second encounter has not happened yet. Profiles of surface brightness of NGC 7769 have a characteristic break, and profiles of color indices have a minimum at a radius of intensive star formation induced by the interaction with NGC 7771.

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Section: Description Of the Systemsupporting

confidence: 88%

Hα Velocity Fields and Galaxy Interaction in the Quartet of Galaxies NGC 7769, 7770, 7771 and 7771A

2016

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“…According to the nearby SN rates estimated by Maoz et al (2011), a young star burst (<420 Myr) produces ten times more CC SNe than SNe Ia. Although a few CC SNe have been observed in elliptical galaxies that show signs of star formation from UV observations (e.g., Hakobyan et al 2008;Suh et al 2011), they are much rarer than SNe Ia. Therefore, at least part of SNe Ia probably come from old SPs, as demonstrated by Maoz et al (2011.…”

Section: Correlation To Star-forming Regionsmentioning

confidence: 92%

Nearby supernova host galaxies from the CALIFA Survey

Galbany

Stanishev²,

Mourão³

et al. 2014

A&A

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We use optical integral field spectroscopy (IFS) of nearby supernova (SN) host galaxies (0.005 < z < 0.03) provided by the Calar Alto Legacy Integral Field Area (CALIFA) Survey with the goal of finding correlations in the environmental parameters at the location of different SN types. In this first study of a series we focus on the properties related with star formation (SF). We recover the sequence in association of different SN types to the star-forming regions by using several indicators of the ongoing and recent SF related to both the ionized gas and the stellar populations. While the total ongoing SF is on average the same for the three SN types, SNe Ibc/IIb tend to occur closer to star-forming regions and in higher SF density locations than SNe II and SNe Ia; the latter shows the weakest correlation. SNe Ia host galaxies have masses that are on average ∼0.3−0.8 dex higher than those of the core collapse (CC) SNe hosts because the SNe Ia hosts contain a larger fraction of old stellar populations. Using the recent SN Ia delay-time distribution and the SFHs of the galaxies, we show that the SN Ia hosts in our sample are expected to produce twice as many SNe Ia as the CC SN hosts. Since both types occur in hosts with a similar SF rate and hence similar CC SN rate, this can explain the mass difference between the SN Ia and CC SN hosts, and reinforces the finding that at least part of the SNe Ia originate from very old progenitors. By comparing the mean SFH of the eight least massive galaxies with that of the massive SF SN Ia hosts, we find that the low-mass galaxies formed their stars during a longer time (0.65%, 24.46%, and 74.89% in the intervals 0-0.42 Gyr, 0.42-2.4 Gyr, and >2.4 Gyr, respectively) than the massive SN Ia hosts (0.04%, 2.01%, and 97.95% in these intervals). We estimate that the low-mass galaxies produce ten times fewer SNe Ia and three times fewer CC SNe than the high-mass group. Therefore the ratio between the number of CC SNe and SNe Ia is expected to increase with decreasing galaxy mass. CC SNe tend to explode at positions with younger stellar populations than the galaxy average, but the galaxy properties at SNe Ia locations are one average the same as the global galaxy properties.

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“…Figure 15 presents the cases of CC SNe in early-type hosts. Hakobyan et al (2008) already reported and investigated in detail two cases of such CC SNe in early-type galaxies (2000ds (Filippenko & Chornock 2000) has been confirmed to be an S0, with a central region showing dust and a disky central gas distribution (e.g., Hakobyan et al 2008). According to the outer isophotal structure and radial surface brightness profile of the host of SN 2006ee (Puckett et al 2006), this must be an S0 galaxy.…”

Section: Distribution Of Sn Typesmentioning

confidence: 93%

“…They suggested that to understand the dependence of SN type on the host galaxy population, it is more important to obtain accurate morphological classifications than it is to increase the size of the sample. For example, among ∼800 morphologically classified hosts of CC SNe, Hakobyan et al (2008) found 22 cases where the host had been classified as E or S0. Following a detailed morphological analysis, they found that among these 22 early-type objects, 17 are in fact misclassified spiral galaxies, one is a misclassified irregular, and one is a misclassified ring galaxy, leaving only 3 early-type galaxies 15 .…”

Section: Comparison Of Host Galaxy Morphological Classificationsmentioning

confidence: 99%

Supernovae and their host galaxies

Hakobyan

Adibekyan

Aramyan

et al. 2012

A&A

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Context. In this first paper of a series, we report the creation of large and well-defined database that combines extensive new measurements and a literature search of 3876 supernovae (SNe) and their 3679 host galaxies located in the sky area covered by the Sloan Digital Sky Survey (SDSS) Data Release 8 (DR8). Aims. This database should be much larger than previous ones, and should contain a homogenous set of global parameters of SN hosts, including morphological classifications and measures of nuclear activity. Methods. The measurements of apparent magnitudes, diameters (D 25 ), axial ratios (b/a), and position angles (PA) of SN host galaxies were made using the images extracted from the SDSS g-band. For each host galaxy, we analyzed RGB images of the SDSS to accurately measure the position of its nucleus to provide the SDSS name. With these images, we also provide the host galaxy's morphological type, and note if it has a bar, a disturbed disk, and whether it is part of an interacting or merging system. In addition, the SDSS nuclear spectra were analyzed to diagnose the central power source of the galaxies. Special attention was paid to collect accurate data on the spectroscopic classes, coordinates, offsets of SNe, and heliocentric redshifts of the host galaxies. Results. Identification of the host galaxy sample is 91% complete (with 3536 SNe in 3340 hosts), of which the SDSS names of ∼1100 anonymous hosts are listed for the first time. The morphological classification is available for 2104 host galaxies, including 73 (56) hosts in interacting (merging) systems. The total sample of host galaxies collects heliocentric redshifts for 3317 (∼90%) galaxies. The g-band magnitudes, D 25 , b/a, and PA are available for 2030 hosts of the morphologically classified sample of galaxies. Nuclear activity measures are provided for 1189 host galaxies. We analyze and discuss many selection effects and biases that can significantly affect any future analysis of our sample. Conclusions. The creation of this large database will help to better understand how the different types of SNe are correlated with the properties of the nuclei and global physical parameters of the host galaxies, and minimize possible selection effects and errors that often arise when data are selected from different sources and catalogs.

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Early-type galaxies with core collapse supernovae

Cited by 51 publications

References 79 publications

Hα Velocity Fields and Galaxy Interaction in the Quartet of Galaxies NGC 7769, 7770, 7771 and 7771A

Hα Velocity Fields and Galaxy Interaction in the Quartet of Galaxies NGC 7769, 7770, 7771 and 7771A

Nearby supernova host galaxies from the CALIFA Survey

Supernovae and their host galaxies

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