HUNTING FOR HIDDEN SUPERNOVAE · HUNTING FOR HIDDEN SUPERNOVAE Jacob Jencson The...
Transcript of HUNTING FOR HIDDEN SUPERNOVAE · HUNTING FOR HIDDEN SUPERNOVAE Jacob Jencson The...
HUNTING FOR HIDDEN SUPERNOVAEJacob Jencson The Progenitor-Supernova-Remnant Connection Caltech Astronomy Ringberg CastleAdvisor : Mansi Kasliwal July 25, 2017
July 25, 2017Jacob Jencson 2/16
Optical searches are blind to supernovae heavily obscured by dust.
IR searches can provide a way forward, but have been hindered by detector cost and the bright IR night sky background.
Transient surveys now coming online will systematically explore the dynamic infrared sky.
Image Credit: NASA, ESA, A. Goobar (Stockholm University), and the Hubble Heritage Team (STScI/AURA)
July 25, 2017Jacob Jencson 3/16
Open Questions:
1. What is the missing SN fraction in the local universe?• Can obscured SNe explain the “supernova rate problem?”
2. What are the progenitors of obscured SNe?• Can obscured SNe explain the “red supergiant problem?”
3. What are the environmental conditions of obscured SNe? • Do obscured SNe represent a separate SN population
originating from extreme environmental conditions?
July 25, 2017Jacob Jencson 4/16
Previous searches have focused on extreme environments of (U)LIRGs and starbursts.
SN 2004ip in IRAS 18293-3413
16.5’’ x 11.5’’
2004 Sept. 15NACO Ks-band
Image subtraction with May 4 reference.
4 confirmed obscured SNe from near-IR, high-resolution searches (Cresci+ 2007, Mattila+ 2007, Kankare+ 2008, 2012).
Radio VLBI studies reveal scores of missed SNe (e.g., Perez-Torres+ 2009, Romero-Cañizales+ 2012).
No candidates from Spitzer search of nearby starbursts (PI O. Fox). Mattila+ 2007
2004 Sept. 15
July 25, 2017Jacob Jencson 5/16
SPIRITS: A targeted search of nearby galaxies for transients in the mid-IR.1410 hours over 5 years with Spitzer
Cycles 10-12 (2014-2016)194 galaxies x 10 epochs
Cycle 13 (2017-2018)105 galaxies x 4 epochs
Sample < 20 Mpc
Depth of 20 mag (Vega) at [3.6] and 19 mag at [4.5]
Cadence baselines spanning one week to several years
SPIRITS Team: M Kasliwal, J Jencson, S Adams, R Lau, S Tinyanont, D Perley, F Masci, G Helou, L Armus, S Van Dyk, A Cody, M Boyer, H Bond, A Monson, J Bally, O Fox, R Williams, P Whitelock, R Gehrz, N Smith, J Johansson, E Hsiao, M Phillips, N Morell, C Contreras+
July 25, 2017Jacob Jencson 6/16
SPIRITS is discovering a wide range of IR transient sources.
Identified147+ transients:•37 known supernovae•17 likely novae•57 eSPecially Red
Intermediate-Luminosity Transient Events (SPRITEs; Kasliwal+ 2017)
10 luminous transients are likely to be newly discovered obscured SNe.ATels: Kasliwal+ 2014: #6644
Jencson+ 2015-17: #7929, 8688, 8940, 9434, 10171, 10172, 10488
July 25, 2017Jacob Jencson 7/16
Fraction of missed obscured events may be as high as 50%.
14azy 14bug 15c, 14buu
15mr 15ud 15ade
16aj16ix 16tn
Equal number of optically discovered CCSNe in our sample since 2014
Two confirmed spectroscopically, and one additional based on optical/near-IR light curves (Jencson+ 2017; Jencson+ in prep.)
Radio follow-up with VLA and ATCA ongoing
& 17lb
July 25, 2017Jacob Jencson 8/16
SPIRITS 16tn: a highly obscured, probable CCSN at only 9 Mpc.
Jencson+ in prep.
Spitzer/IRAC [4.5] 2016 Aug. 15
Spitzer/IRAC [4.5] 2011 Feb. 7
Sci. Ref. Sub.
Messier 108
SDSS
Swift/UVOT UBV 2016 Aug. 29
−22
−20
−18
−16
−14
−12
[4.5]a
bsol
ute
mag
nitu
de(V
ega)
Type II
Ic/IIn
Types IIb & Ib/c Type Ia
Ia-CSM
Iax
0 100 200 300 400Time (days)
−1
0
1
2
3
[3.6]−
[4.5](
Vega
mag
)
0 100 200 300 400Time (days)
0 100 200 300 400Time (days)
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SPIRITS 16tn is unique in its mid-IR properties.
Jencson+ in prep.
SPIRITS 16tn
SN 2008S
July 25, 2017Jacob Jencson 10/16
Near-IR spectrum rules out an SN Ia.
1.4 1.6 1.8 2.0 2.2 2.4Rest wavelength (µm)
0
5
10
15
Normalized
flux+constant
SN 1998bw(Ic-BL)60 days
SN 2010jl (IIn)178 days
SN 2011dh (IIb)205 days
SN 2013ej (IIP)138 days
SPIRITS 16tn136 - 218 days
He IMg I [Fe II]+ [Si I]
Br γ
1.50 1.55 1.60 1.65 1.70 1.75 1.80Restwavelength (µm)
0
2
4
6
8
10
Normalized
flux+constant
SN 2014J128 days
SN 2005df198 days
SN 2005df217 days
SN 2005df380 days
SPIRITS 16tn136 - 229 days
[Fe
II]
[Co
II]
[Co
III]
[Fe
II] [Fe
II]
[Fe
II] [C
oII
][F
eII
]
[Co
II]
Jencson+ in prep.
July 25, 2017Jacob Jencson 11/16
Comparisons with Type II SN suggest AV ~ 7 - 9 mag.
−16
−14
−12
−10
−8
−6
Abs
olut
em
agni
tude
(Veg
a)
−200 −100 0 100 200 300Days since earliest detection
12
14
16
18
20
22
24
App
aren
tmag
nitu
de(V
ega)
U
B
V
I
z
J
HKs
[3.6]
[4.5]
0.5 1.0 5.0λ (µm)
104
105
106
107
λLλ
(L⊙
)
SPIRITS 16tnt ∼ 40–125 days
SN 2004et×(3.7× 10−2)
t = 140 days
with AV = 8.4 mag,
E(B − V ) = 2.7 mag
U B BB I J H Ks [3.6] [4.5]
Jencson+ in prep.
July 25, 2017Jacob Jencson 12/16
VLA and AMI radio non-detections suggest a weak event or significant absorption.
100 101 102 103
tpeak (days)× (ν/5 GHz)
1024
1025
1026
1027
1028
1029
Lν,peak(erg
s−1Hz−
1 )
Type IIType IInType IIbTypes Ib/cSPIRITS 16tn
Figure adapted from Romero-Cañizales+ 14.
Jencson+ in prep.
July 25, 2017Jacob Jencson 13/16
No detection of the progenitor star in archival optical HST imaging.
Jencson+ in prep.
Background figure: Smartt 15
July 25, 2017Jacob Jencson 14/16
SPIRITS 14buu, 15c, & 17lb: 3 SNe in 4 years in IC 2163.
Jencson+ 2017
100
200SPIRITS ([4.5])
2 5 10 20 50 100 200Distance (Mpc)
0
5
10
15
20
25A
V(m
ag) PG-IR (J)
ZTF (i)
July 25, 2017Jacob Jencson 15/16
A combination of IR searches will be sensitive to obscured SNe at a range of distances.SPitzer InfraRed Intensive Transients Survey (SPIRITS):
• 3.6 and 4.5 μm targeted survey of nearby galaxies.
Palomar Gattini-IR (PG-IR):• Nightly J-band survey of
15000 deg2.• Expect ~ 13 SNe within 50
Mpc in 1 year.
Zwicky Transient Facility (ZTF):
• i-band survey of 6700 deg2 at 4-day cadence.
• Expect ~ 50 CCSN within 100 Mpc in 1 year.
Jencson+ in prep.
July 25, 2017Jacob Jencson 16/16
SummaryOptical searches for SNe may miss events heavily obscured by dust.
SPIRITS is an ongoing search for transients in the mid-IR, and has found 10 dust obscured SN candidates thus far.
SPIRITS 16tn, our nearest candidate at only 9 Mpc, is a probable low-energy SN, though its mid-IR properties are unique among previously studied events.
With upcoming surveys in the optical and near-IR, we can systematically search for reddened SNe and obtain spectroscopically complete samples across varying levels of obscuration.
Searching for and characterizing obscured SNe will allow us to probe their significance for the missing SN fraction, and whether these events represent a separate population originating from extreme environmental conditions and progenitor systems.