Ashley Pagnotta very old novae Ben Oppenheimer chemistry of hot Jupiter atmosphere MS Dave Zurek Magellanic dwarf novae Adric Reidel young red dwarfs Jackie ID: 589382
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Slide1
AMNH SALT SCIENCE
Ashley
Pagnotta
(very old novae),
Ben Oppenheimer (
chemistry of hot Jupiter atmosphere)
,
MS + Dave
Zurek
(
Magellanic
dwarf novae)
Adric
Reidel
(young
red
dwarfs)
Jackie
Faherty
(brown dwarf rotations)
June
6/
2014Slide2
Pagnotta
:Eventually, we will produce long term light curves for all known galactic classical novae, such as this one for V603 Aquilae. Our light curves will be anchored by modern magnitudes from SALT and other sources.Slide3
BV Cen is a U Gem/SS
Cyg-type dwarf nova that has shown an increase in the time between its DN outbursts over the past half century, indicating a decrease in the accretion rate and possible nova eruption in its past.
Plummer & Horn (2009)Slide4
We used SALTICAM
on BV Cen to obtain a total of 30 minutes of integration time using the Hα filter to search for a nova shell; none present.
2014-1-AMNH-002
BV CenSlide5
Additionally, we continue our survey of modern magnitudes of post-nova systems, searching for evidence of secular change that may confirm or challenge the hibernation theory, for example with V604
Aquilae.
2014-1-AMNH-003
B
g
’
r’Slide6
Shara and
ZurekDwarf Novae and Old Novae in the LMC – 9 epochs over 2 months u and
g
filters
sdss
g
sdss
u
Note Gradients across imagesSlide7
~40 IMAGES IN EACH FILTER ARE DITHERTED
CO-ADD IMAGES, BUTHIGH DATA VALUES (i.e. stars) REJECTED
sdss
u
sdss
gSlide8
FLATTENED, COSMIC-RAY CLEANED, COSMETICALLY CLEANED, ALIGNED, CO-ADDED IMAGES
u ~g ~25… deep enough to detect quiescent cataclysmic variables
Large amplitude blue variables seen
between epochsSlide9
~1% of the stars are very blue (
u-g < 0)The most variable are cataclysmic binaries
sdss
u
sdss
u-gSlide10
Oppenheimer: Measurement
of Wasp 43b Transit SpectrumThe hottest transiting
exoplanet
Period = 19.52 hours
M =~ 2 x Jupiter R ~ R(Jupiter
)
semimajor
axis = 0.014 AUMstar = 0.58
MsunGoal : Transmission spectrum of the planet’s atmosphereINITIAL Method: {Star alone} - {Star minus Planet} =Planeti.e. Primary transit spectrum minus secondary transit spectrum =PLANET ATMOSPHERE SPECTRUM
ULTIMATE GOAL: SPECTROPOLARIMETRY AROUND THE ORBIT
SALT RSS
longslit
pg0900 grating data on
1-15 and 2-06 of 2014
in transit and out of transit 1200 seconds exposure In process of reducing above data.Slide11
1.15.14 22:49
1.15.14 22:14
Observations: 1 (300.2s) 22:42:23 - 22:47:23 5 (300.2s) 23:03:41 - 23:08:41
2 (300.2s) 22:47:43 - 22:52:43 6 (300.2s) 23:09:00 - 23:14:00
3 (300.2s) 22:53:02 - 22:58:02 7 (300.2s) 23:14:20 - 23:19:20
4 (300.2s) 22:58:21 - 23:03:21 8 (300.2s) 23:19:39 - 23:24:39
34
33
32
31
30
29
28
27Slide12
2.06.14 21:22
2.06.14 21:57
Observations: 1 (300.2s) 21:42:51 - 21:47:51
2 (300.2s) 21:48:10 - 21:53:10
3 (300.2s) 21:53:30 - 21:58:30
4 (300.2s) 21:58:50 - 22:03:50
12
13
14
15Slide13
Un-calibrated Results
Wasp 43 b in transit spectra
Wasp 43b out of transit spectra
Difference SpectrumSlide14
Next Steps
Apply instrument function to the dataIdentify possible lines in the spectrum…NaI 5889 AngstromsOr evidence of broadband scattering and cloud coverSlide15
Expect ~2-3 AMNH
papers in the coming 6 months