Collaborators
Swift/UVOT SNe Group•Pete Roming (Advisor)•Amanda Bayless•Peter Brown•Stephen Holland•Stefan Immler•Peter Milne•Sam OatesLANL•Wesley Evan
•Lucy Frey
•Chris Fryer

CSP• Joe Anderson• Max Stritzinger

Outline Background Swift observations of Core Collapse SNe UV-NIR Studies

Type IIP SNe
Smartt	  2009	
  Plateau driven by Hydrogen recombination wave
© Swinburne University of Technology

Why UV?

Bersten+ 09

Dessart & Hillier 10-Lots of Flux -O/Fe/Ni -Extinction-Rapid Evolution

UV Variation Impact on Bolometric LC

 At these early times, for UV bright SNe, progenitor
differences appear more clearly in the UV
23 solar Mass, 5x1050 erg KE, 10-5/10-6 (A/B) progenitor mass loss
Also,	
  see	
  Frey+2013,	
  Bayless+2013	  Drastic Increase in SNe Obs
Number of Supernovae Discovered by Year

# SNe Discovered

1000

100

 SNe observations peryear Increased by anorder of magnitude inthe late 50’s
 Again in the 1990’s

SN 1954aa

 Mostly due to robotic
searches

SN 1954Z
10

 Mostly Optical, Some
more recently have IR01900

19201940 1960
Year19802000

UV Studies of SNe But, UV studies
historically lag behind
optical observations
 Constrained byavailable
instrumentation

Swift – Gamma Ray Burst Finder US, UK, and Italian Collaboration
 Swift – adj. quick Also a type of bird (Swallow)

 Primary Science Goal: Gamma Ray Burst Detection & Followup

 Secondary science goals:
 Transient Science (Supernovae, novae,SSXRB/FXRT) UV, X-ray observations
 UV, X-Ray Great Observatory Support

GRB (Transient) Hunter Rapid response capability – Targets of Opportunity
can be uploaded to the spacecraft for immediateobservation
 Short term scheduling, required by the different
behavior of burst afterglows, requires observations
to be planned the day before rather than weeks inadvance SN observations can be analyzed in near real time(hours delay from observation to analysis) to assistin planning the future observations
 Unique UV and X-ray observations unobtainablefrom the groundThe NASA Swift Satellite Mission
 Launched November 20, 2004
 Low earth orbit with ~90 min period
 Three co-aligned instruments
 BAT – Burst Alert Tel. (15-150 keV) XRT – X-Ray Telescope (0.2-10 keV) UVOT - UltraViolet/Optical TelescopeSwift/UVOT 30 cm modified Ritchey-Chretien Telescope Wavelength Range 1600-6000 Angstroms
 Photon Counting detector centroiding into 0.5 arcsec
virtual pixels
 2 arcsec point spread function
 17x17 arcminute field of view

Swift Supernovae Program Open Observatory:
 TOO:
http://www.swift.psu.edu/too.html
 Also, Annual Fall proposal cycle for non time-criticalobservations

 Collaborative effort with ground-based SNe Discovery &Observation Groups Targets chosen from those found by robotic search groups andannounced over IAUC/CBET/ATEL Informal email list to coordinate observations
 Targets chosen to maximize science and UV/X-Ray observationsYoung (the earlier, the better)
Nearby (z<0.02)
Low Line of Sight Extinction
5-10” Separation from Galactic nucleus

8 Years of Swift SNe Observations …

NASA/Swift/S. Immler

Swift/UVOT Filters

λc
uvw2:
uvm2:
uvw1:

Å19282246
2600

Poole+ 08

UV-NIR Coverage
Normalized Throughput

1.015,000K 10,000K
W2 M2 W1UVU u

5,000K
Bg V ri

3,000KY JH

 Combine UVOT and
CSP I Optical/NIR Data λ	 ≈ 1800-18000 Å0.8

 Swift/UVOT

0.6

 uvw1,uvm2,uvw1,u CSP I0.4

 ugriBVYJH

0.2

0.0
2000

10000
Wavelength (Angstroms)

Swift+CSP I SNe
SN 2006bc H
JY

H
JYV
B
i
r
guuvu
uvw1
uvm2
uvw2

182016VB
irgu18

3840
3860
3880
Julian Date 2450000+

3900

4400

4420

4440
4460
4480
Julian Date 2450000+

4500

SN 2009N

Magnitude

Magnitude

1618

16HJY

18

V
B
i
rguuvu
uvw1
uvm2
uvw2

20

20

uvw1
uvw1
uvm2
uvw2

224480

HJ
Y4500

i
rguV
B

4520
4540
4560
Julian Date 2450000+

224580

4600

HJY

18

V
B
i
r
gu
uvu
uvw1
uvm2
uvw2

22

14

SN 2008M

1620

uvu
uvw1
uvm2
uvw2

20

223820SN 2008aw

14

Magnitude

Magnitude16

14

SN 2007od

Magnitude

14

4860 4880 4900 4920 4940 4960 4980 5000
Julian Date 2450000+

4550

4600
4650
Julian Date 2450000+

4700

Bolometric Light Curves

Normalized Throughput

1.015,000K 10,000K
W2 M2 W1UVU u

5,000K
Bg V ri

3,000KY J

UV Correction =
integral of all
wavelengths blueward of bluest
observed
wavelength

H

0.8

0.6

∞

0.4

IR Correction =
integral of all
wavelengths redward of reddest
observed
wavelength

0.2

IR Correction

0.0

UV
2000
Correction

10000
Wavelength (Angstroms)SN 2012aw#$"()*+$'$&$%!!!!!uvw2!!!!!uvm2!!!!!uvw1!!!!!u!!!!!b!!!!!v

"#& !

!

!

!

!
!!!!!uvw2ïuvm2!!!!!uvm2ïuvw1!!!!!uvm2ïv!!!!!bïv'6(!

"#
ï"
#

"#'#
&#%#$##,-.+!/0123!4567)+0)1!89,!"':&##";:<

Bayless+ 13

Flux Completeness87!

~85-90%+ flux completion(when observations overlap)

9:'.;,<-*<=*>65,-<),;(!7%!7$"!!$1.
"!!?<2"!!%3"!!%'@"!!AB

!7#

C0DE
F+G

!7"!7!
!

"!
#!
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%!
&'()*+,-./*0ï1'-2*3'4,565

UVOT+CSP Bolometric Light Curves•Early Linear decay
SN 2006bc
SN 2007od
SN 2008M
SN 2008aw
SN 2009N

Luminosity [ergs/s]

10431042

020406080Days Since V−band Maximum•Variability in bolometric plateau
Length/Shape?
•2009N: sub-luminous object

UV Corrections (From UV-NIR Data)
)
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--/
---&-&-0

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,-.

*+,

(+123!##)&0
123!##456
123!##78
123!##79:
123!##;2

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345%##678
345%##9:345%##9;<345%##=4%

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Why is u so much better?

u -O/Fe/Ni vs H/He(non SCCSNe)bDessart & Hillier 10

Summary
 UV Observations important at early times
 Information on total energetics, metalicity
 UV behavior heavily dependant on subtype

 Neglecting UV Flux in bolometric calculations can bedangerous (Ground based u-band can be a good diagnostic of this) We can supply an empirical correction for UV Flux
 Understanding the locally observed UV flux will be
important for interpreting results from future high-z
synoptic survey programs (LSST, etc)
 Variable Extinction, metallicity, stellar structure …