−10 0 10 20 Dec[arcsec] −10 0 10 20 Dec[arcsec] 1993R 2014cy

2014cy
1993R
SUPERNOVA ENVIRONMENTAL STUDIES
THROUGH INTEGRAL FIELD SPECTROSCOPY
Lluís Galbany
Fondecyt Fellow (U. Chile)
4 kpc
Direct progenitor detection in pre-explosion images
Why SN environments?
CCSNe
Stellar evolution
(progenitors)
Anderson, Modjaz, Prieto, Leloudas,
Smartt, Sorderberg, Follatelli, Pignata...
SNeIa
Cosmology
Improve standardization
adding host/environment properties
Reduce systematic errors
Sullivan, Kelly, Howell, Lampeitl,
Hamuy, D’Andrea, Gallagher...
•
Global properties
photometry / imaging
(Sullivan+10, Lampeitl+10, Anderson+09…)
single-aperture /long-slit spectroscopy (@galaxy core)
(Prieto+08, D’Andrea+12…)
•
Local properties
central values + gradients
(Boissier+09, Galbany+12…)
single-aperture / long-slit spectroscopy (@SN position)
(Anderson+10&12, Modjaz+11…)
I
Integral Field Spectroscopy
The Calar Alto Legacy Integral Field Area (CALIFA) survey
•
survey of ~600 galaxies of all types at
z=0.005 to 0.03
•
diameter selected from SDSS DR7, 45 < D25 < 80, to fit in the IFU FOV
CALIFA mother sample: 939 galaxies
•
IFS using PPAK @ 3.5m CAHA
2 setups: mid (V500) and high-res (V1200)
spectral coverage [3700-7000 A]
spatial resolution ~1 arcsec
FoV ~1’ x ~1’
•
•
~3000 spectra per galaxy
data has been already freely distributed
to the community:
DR1 (100 galaxies), husemann+13
DR2 (200 galaxies), garcía-benito+15
DR3 (670 galaxies), sánchez+16
Analysis
1- continuum fit with single stellar
population (SSP) models and
STARLIGHT:
CB07:
17 Ages 106 to 1.8 1010 M
4 metallicities 0.004, 0.05, 0.2, 2.5 Z
(Z =0.02)
Fλ (× 10−17 erg s−1 cm−2 Å−1)
8
AV = 0.27
<log(t∗)>M = 9.98
<log(t∗)>L = 8.65
<Z>M = 0.027
<Z>L = 0.007
60
50
40
30
20
10
0
10
5
3 - get REAL integrated (total)
spectra, deprojected maps using
Ha velocity field
0
6
6
2- construct strong line emission
maps by fitting gaussians to the
pure emission spectra
15
xi [%]
10
µi [%]
Fit range: [3660:7000] Å
7
8
9
log(t∗) [yr]
10
6
7
8
9
log(t∗) [yr]
10
4
2
0
4000
4500
5000
5500
Rest wavelegth [Å]
6000
6500
7000
Analysis
NGC 4210
Analysis
FH`
NGC 4210
Analysis
FH`
vH`
NGC 4210
Analysis
FH`
vH`
v*
NGC 4210
Analysis
FH`
vH`
v*
<t*>
NGC 4210
Analysis
FH`
vH`
v*
<t*>
OIII/Ha
NGC 4210
Analysis
FH`
vH`
v*
<t*>
OIII/Ha
BPT
NGC 4210
Analysis
FH`
vH`
v*
<t*>
OIII/Ha
BPT
AV
NGC 4210
Analysis
FH`
vH`
v*
<t*>
OIII/Ha
BPT
AV
O/H
NGC 4210
Analysis
FH`
vH`
v*
<t*>
OIII/Ha
BPT
AV
O/H
DSFR
…
NGC 4210
Sample
c ESO 2
Astronomy & Astrophysics manuscript no. IFU_P1_v9
September 17, 2014
cross-check SNe IAU list with CALIFA galaxies (by coord.)
Nearby supernova host galaxies from the CALIFA Survey:
I. Sample, data analysis, and correlation to star-forming regions
L. Galbany1, 2, 3 , V. Stanishev1 , A. M. Mourão1 , M. Rodrigues4, 5 , H. Flores5 , R. García-Benito6 , D. Mast7 ,
M. A. Mendoza6 , S. F. Sánchez8 , C. Badenes9 , J. Barrera-Ballesteros10, 11 , J. Bland-Hawthorn12 ,
J. Falcón-Barroso10, 11 , B. García-Lorenzo10, 11 , J. M. Gomes13 , R. M. González Delgado6 , C. Kehrig6 ,
M. Lyubenova14 , A. R. López-Sánchez15, 16 , A. de Lorenzo-Cáceres17 , R. A. Marino18 , S. Meidt13 , M. Mollá19
P. Papaderos13 , M. A. Pérez-Torres6, 20, 21 , F. F. Rosales-Ortega22 , G. van de Ven14 , and the CALIFA Collaboratio
(Affiliations can be found after the references)
Received 31 July 2014 / Accepted 4 Setember 2014
ABSTRACT
ronomy & Astrophysics manuscript no. IFU_P2_v4
ril 6, 2015
We use optical integral field spectroscopy (IFS) of nearby supernova (SN) host galaxies (0.005 < z < 0.03) provided by the Calar Alto
c ESO
2015Field Area (CALIFA) Survey with the goal of finding correlations in the environmental parameters at the location of
Legacy
Integral
di↵erent 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 di↵erent 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 on average are ⇠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 di↵erence 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
Collaboration
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.
Nearby supernova host galaxies from the CALIFA Survey:
II. SN environmental metallicity
L. Galbany1, 2 , V. Stanishev3 , A. M. Mourão3 , M. Rodrigues4, 5 , H. Flores5 , and the CALIFA
(Affiliations can be found after the references)
Received ————- / Accepted ————-
Key words.
stellar content
Galaxies: general – techniques: spectroscopic – (Stars:) supernovae: general – galaxies: star formation – galaxies:
ABSTRACT
1. Introduction
We present the second study using optical Integral Field Spectroscopy (IFS) of nearby supernova (SN) host galaxies (0.005 < z < 0.03)
to characterize the environmental parameters at the location of di↵erent SN types. We increased the sample from Galbany
et al. (2014)
Supernova
(SN) explosions are one of the key processes that
with 29 objects, which makes a total sample of 125 SNe of all types in 110 galaxies. In this work we focused ondrive
studying
the SN evolution of galaxies. Throughout their lifethe chemical
environmental metallicities, for which wide-field IFS enables proper comparisons of di↵erent approaches. Using the
O3N2
calibrator
time,
stars
fuse lighter into heavier chemical elements in their
from Marino et al. (2013), we found that the average metallicity at the location of SNe Ia is higher than at the position
of
CC
cores, andSNe
the by
explosion at the end of a star’s life is responsible
0.05 dex, being similar but slightly higher for Ibc than for SN II. While the central and total metal abundances are similar for CC SN
for dispersing the newly synthesized heavy elements into the inand SNIa hosts, the stellar metallicity of SN Ia host is significantly higher than that of CC SN host galaxies (< Z>⇠ 0.010). When
terstellar
medium
the AGN contribution is excluded from the total spectra, the average metallicity of the SNe Ia host galaxies is 0.03
dex higher
than (ISM). The next generation of stars form from
gas
that
has
already been enriched by heavier elements. Thus,
the measured not excluding the AGN. This can be interpreted as a systematic e↵ect when measuring metallicities of galaxies which
starting
from
gas consisting of only H, He, and a tiny fraction of
structure cannot be resolved (dwarf galaxies at lower redshifts or any galaxy at higher redshifts). By comparing the SN environmental
Li, the heavy-element content of galaxies gradually increases to
collapse SNe (CC SNe). The end product of stars with m
between ⇠0.5 and 8 M is a degenerate carbon-oxygen (
white dwarf (WD) (Becker & Iben 1980). The upper mass
of C/O WDs is ⇠ 1.1 M (Dominguez et al. 1999), but if
a star can increase its mass to ⇠1.4 M , thermonuclear reac
can ignite in the center and the WD can be completely disru
in a very bright thermonuclear explosion that leads to a ty
SN (SNe Ia, Hoyle & Fowler 1960). CC SNe disperse
amounts of intermediate mass elements (IME) such as oxyg
carbon, but most of the synthesized iron-group elements re
Star formation rate at SN locations
1.0
1.0
II - 33
Ibc/IIb - 20
Ia (all) - 42
Ia (active) - 35
0.8
local
0.6
Fraction of SNe
Fraction of SNe
0.8
0.4
0.2
0.0
-2.0
total
-1.5
-1.0
-0.5
0.0
0.5
log10(SFR [MO• yr-1])
1.0
0.6
0.4
1.5
0.2
Even in galaxies with similar SFR, Ibc/IIb
tend to explode in higher DSFR regions
than II and Ia
II − 33
Ibc/IIb − 20
Ia (active) − 35
total galaxy
Fraction of SNe
Fraction of SNe
0.8
0.6
0.4
0.2
0.0
7.0
1.0
1.0
0.8
0.8
0.6
0.4
0.2
7.5
8.0
8.5
9.0
<log (t*/yr)>
9.5
10.0
-3
-2
-1
-1
-2
log10 (Σ SFR [MO• yr kpc ]) at SN position
Fraction of SNe
1.0
0.0
-4
II - 33
Ibc/IIb - 20
Ia (all) - 42
Ia (active) - 35
0.0
10.5
0
II − 33
Ibc/IIb − 20
Ia (active) − 35
total galaxy
20
40
60
80
Percent young stellar popullations
0
0.6
0.4
0.2
0.0
100
0
II − 33
Ibc/IIb − 20
Ia (active) − 35
total galaxy
20
40
60
Hα equivalent width [A]
80
100
Local host galaxy properties - star forming regions
1.0
Fraction of SNe
0.8
0.6
0.4
0.2
0.0
0.0
Ia (all) − 42
Ia (SF) − 35
Ib/c − 20
II − 33
0.5
1.0
1.5
Distance to the nearest HII region [kpc]
2.0
SN environments in the submillimeter
NGC 2906 − log(Hα flux)
−14.8
EDGE survey
CO observations of 175 CALIFA galaxies
using CARMA with 2 configurations D+E
Dec[arcsec]
20
CO 1
0
0 (2.6mm) intensity maps
23 SN host galaxies (26 SNe)
−20
2 kpc
1.0
−18.0
20
0
R.A.[arcsec]
−20
0.8
NGC 5056 − log(Hα flux)
Fraction of SNe
−15.0
Dec[arcsec]
20
0.6
0.4
0
Local
Ia − 7
Ibc/IIb − 7
II − 12
0.2
−20
0.0
−2.0
2 kpc
−18.0
20
0
R.A.[arcsec]
−20
−1.5
−1.0
log10 (SCO [Jy km s−1])
−0.5
SN environments in the submillimeter
NGC 2906 − log(Hα flux)
−14.8
EDGE survey
CO observations of 175 CALIFA galaxies
using CARMA with 2 configurations D+E
Dec[arcsec]
20
CO 1
0
0 (2.6mm) intensity maps
23 SN host galaxies (26 SNe)
−20
2 kpc
1.0
−18.0
20
0
R.A.[arcsec]
−20
0.8
NGC 5056 − log(Hα flux)
Fraction of SNe
−15.0
Dec[arcsec]
20
0.6
0.4
0
Local
Ia − 7
Ibc/IIb − 7
II − 12
0.2
−20
0.0
0.0
2 kpc
−18.0
20
0
R.A.[arcsec]
−20
0.5
1.0
1.5
AV,gas [mag]
2.0
Metallicity gradients
NGC4961 − 12+log(O/H)R13,O3N2
8.60
0.0
8.55
1.0
R (re)
1.5
2.0
0
8.45
8.40
8.35
8.30
−20
4 kpc
8.20
20
0
R.A.[arcsec]
8.25
0
2
0
1
4
R (kpc)
−20
NGC2347 − 12+log(O/H)R13,O3N2
8.70
R (re)
2
12+log(O/H)R13,O3N2
8.6
0
8
3
4
8.5
8.4
−20
6
NGC2347
a = 8.667
b = −0.095
20
Dec[arcsec]
2.5
NGC4961
a = 8.535
b = −0.107
8.50
12+log(O/H)R13,O3N2
Dec[arcsec]
20
0.5
~30%
4 kpc
8.30
20
0
R.A.[arcsec]
−20
0
5
10
R (kpc)
15
Local metallicity
1.0
b) Targeted
0.8
0.6
0.4
Ia − 70
II − 92
Ic − 30
Ib − 28
IIb − 9
Ic−BL − 5
IIn − 35
0.2
0.0
Fraction of SNe
Fraction of SNe
0.8
a) Untargeted
0.6
0.4
Ia − 171
II − 35
Ic − 22
Ib − 18
IIb − 8
Ic−BL − 10
0.2
0.0
8.2
8.3
8.4
8.5
12+log10(O/H) (local)
8.6
8.2
8.3
8.4
8.5
12+log10(O/H) (local)
8.6
Fraction of SNe
1.0
SN environmental studies with IFU <> state-of-the-art
SNIFS + GMOS
PMAS, CALIFA survey
1.0
Fraction of SNe
0.8
0.6
0.4
0.2
0.0
-4
II - 33
Ibc/IIb - 20
Ia (all) - 42
Ia (active) - 35
-3
-2
-1
log10 (Σ SFR [MO• yr-1 kpc-2]) at SN position
0
K13ab: Age and Z of the SN parent cluster.
Small FoV (~6”x6”), high spatial resolution (0.2”x0.2”)
G14: relation between SFR and SN type.
G16: relation between O/H & Z and SN type.
High FoV (1’x1’), low spatial resolution (1”x1”)
See poster
THE AMUSING SURVEY
by Joe
(All-weather MUse Supernova Integral field of Nearby Galaxies)
outside!
•
ALL-WEATHER: makes use of non-optimal weather of
Paranal. Many observations done in bright, THN
conditions (avg. seeing 1.1”, from 0.7” to 1.5”).
•
MUSE: very efficient instrument. 3GB per cube,
>4800 A. Basis for driving big data spectroscopic
astronomy.
•
Supernova: Overall aim is to use MUSE to further
understand supernova progenitors/explosions. Study
SN environment and all other regions within the host.
•
Integral-field: 1’x1' FoV, 0.2” pixel scale. Image-like
resolution but with ‘spaxels’.
•
Nearby: Allows in-depth study of gas and stellar
populations. Classical assumptions for IFU work
break-down.
•
Galaxies: Allows cross-field collaborations. Galaxy
studies: evolution, dynamics, stellar populations…
Aimed to be an open collaboration with regular data releases
including all kinds of data products
See poster
THE AMUSING SURVEY
by Joe
(All-weather MUse Supernova Integral field of Nearby Galaxies)
outside!
•
ALL-WEATHER: makes use of non-optimal weather of
Paranal. Many observations done in bright, THN
conditions (avg. seeing 1.1”, from 0.7” to 1.5”).
•
MUSE: very efficient instrument. 3GB per cube,
>4800 A. Basis for driving big data spectroscopic
astronomy.
•
Supernova: Overall aim is to use MUSE to further
understand supernova progenitors/explosions. Study
SN environment and all other regions within the host.
•
Integral-field: 1’x1' FoV, 0.2” pixel scale. Image-like
resolution but with ‘spaxels’.
•
Nearby: Allows in-depth study of gas and stellar
populations. Classical assumptions for IFU work
break-down.
•
Galaxies: Allows cross-field collaborations. Galaxy
studies: evolution, dynamics, stellar populations…
Aimed to be an open collaboration with regular data releases
including all kinds of data products
See poster
THE AMUSING SURVEY
by Joe
(All-weather MUse Supernova Integral field of Nearby Galaxies)
outside!
•
ALL-WEATHER: makes use of non-optimal weather of
Paranal. Many observations done in bright, THN
conditions (avg. seeing 1.1”, from 0.7” to 1.5”).
•
MUSE: very efficient instrument. 3GB per cube,
>4800 A. Basis for driving big data spectroscopic
astronomy.
•
Supernova: Overall aim is to use MUSE to further
understand supernova progenitors/explosions. Study
SN environment and all other regions within the host.
•
Integral-field: 1’x1' FoV, 0.2” pixel scale. Image-like
resolution but with ‘spaxels’.
•
Nearby: Allows in-depth study of gas and stellar
populations. Classical assumptions for IFU work
break-down.
•
Galaxies: Allows cross-field collaborations. Galaxy
studies: evolution, dynamics, stellar populations…
Aimed to be an open collaboration with regular data releases
including all kinds of data products
THE AMUSING SURVEY TEAM
•
CORE: J. P. Anderson (PI, ESO Chile), L. Galbany (MAS/DAS), T. Kruehler (MPIA)
•
INV.: Chris Ashall (ARI, LJMU), Erik Aquino (UNAM), Subo Dong (Kavli Institute
Beijing U.), Jesús Falcon-Barroso (IAC), Francisco Förster (CMM, U. de Chile),
Santiago Gonzalez-Gaitan (CMM, U. de Chile), Claudia Gutierrez (MAS/DAS/
ESO), Mario Hamuy (DAS/MAS), Tom Holoien (Ohio State U.), Eric Hsiao (U.
Florida), Phil James (ARI, LJMU), Christopher Kochanek (Ohio State U.), Hanin
Kuncarayakti (MAS/DAS), Joe Lyman (U. Warwick), Juan-Carlos Maureira (CMM,
U. de Chile), Enrique Pérez (IAA), Isabel Pérez (U. Granada), Mark Phillips (LCO),
Kara Ponder (U. Pitt.), Jose-Luis Prieto (U. Diego Portales), Alessandro Razza
(MAS/DAS), Fabián Rosales-Ortega (INAOE), Tomás Ruiz-Lara (U. Granada),
Sebastian Sanchez (UNAM), Patricia Sánchez-Blázquez (PUC), Laura SánchezMenguiano (U. Granada), Steve Schulze (MAS/PUC), Ben Shappee (Carnegie
Observatories), Kris Stanek (Ohio State U.), Maximilian Stritzinger (Aarhus U.),
Lingzhi Wang (CASSACA/Calan, U. de Chile), W. Michael Wood-Vasey (U. Pitt.)…
People from both supernova and galaxy communities
and continuously increasing…
MUSE-SV: Pilot study of 6 galaxies that hosted 11 SNe
•
HII region statistics: Distributions of SFR,
oxygen abundance, Av extinction, and EW(Ha)
measured in ALL HII regions in the galaxy, and
characterization of the SN parent HII region.
MUSE-SV: Pilot study of 6 galaxies that hosted 11 SNe
•
HII region statistics: Distributions of SFR,
oxygen abundance, Av extinction, and EW(Ha)
measured in ALL HII regions in the galaxy, and
characterization of the SN parent HII region.
Summary
Summary
Palau de la Música Catalana, Domènech i Muntaner et al. 1908