luhman’16ab · wavelength (!m) 0.6 0.8 1.0 1.2 1.4 1.6 1.8 2.0 absolute f (10 h-17 erg/cm 2 /s/!...
TRANSCRIPT
![Page 1: Luhman’16AB · Wavelength (!m) 0.6 0.8 1.0 1.2 1.4 1.6 1.8 2.0 Absolute F (10 h-17 erg/cm 2 /s/! m) 1.15 1.20 1.25 1.30 1.35 Wavelength (!m) Normalized Flux (F) h QP QP NaP H 2O](https://reader036.vdocuments.us/reader036/viewer/2022071017/5fd070a723f32170701a9535/html5/thumbnails/1.jpg)
Luhman 16AB: A Remarkable, Variable,
L/T Transition Binary at 2 pc
Adam J. Burgasser (UC San Diego) Jacqueline Faherty (U. Chile), Yuri Beletsky (Magellan Obs), Jacqueline
Radigan (STScI), Michael Gillon (U. Liege), Peter Plavchan (Caltech/IPAC), Nidia Morrell (Magellan Obs.), Rachel Osten (STScI), Rachel Street (LCO), Carl Melis (UC San Diego), Amaury Triaud (MIT) & Robert Simcoe (MIT)
![Page 2: Luhman’16AB · Wavelength (!m) 0.6 0.8 1.0 1.2 1.4 1.6 1.8 2.0 Absolute F (10 h-17 erg/cm 2 /s/! m) 1.15 1.20 1.25 1.30 1.35 Wavelength (!m) Normalized Flux (F) h QP QP NaP H 2O](https://reader036.vdocuments.us/reader036/viewer/2022071017/5fd070a723f32170701a9535/html5/thumbnails/2.jpg)
WISE 1049-‐5319AB aka Luhman 16AB
Identified by Luhman (2013) in a proper motion/very cold source search of multi-‐epoch WISE data (2MASS dropouts).
µ = 2.78 “/yr, detection back in 1978
R = 18.6, J = 10.7, Ks = 8.8, W2 = 7.3
b = 5º (are you kicking yourself yet?)
d = 2.02±0.15 pc – 3rd closest system to Sun (closest to α Centauri)
Kinematics nominally consistent with normal field dwarf system, but a suggested association with Argus (Mamajek 2013)
![Page 3: Luhman’16AB · Wavelength (!m) 0.6 0.8 1.0 1.2 1.4 1.6 1.8 2.0 Absolute F (10 h-17 erg/cm 2 /s/! m) 1.15 1.20 1.25 1.30 1.35 Wavelength (!m) Normalized Flux (F) h QP QP NaP H 2O](https://reader036.vdocuments.us/reader036/viewer/2022071017/5fd070a723f32170701a9535/html5/thumbnails/3.jpg)
http://xkcd.com/1212
![Page 4: Luhman’16AB · Wavelength (!m) 0.6 0.8 1.0 1.2 1.4 1.6 1.8 2.0 Absolute F (10 h-17 erg/cm 2 /s/! m) 1.15 1.20 1.25 1.30 1.35 Wavelength (!m) Normalized Flux (F) h QP QP NaP H 2O](https://reader036.vdocuments.us/reader036/viewer/2022071017/5fd070a723f32170701a9535/html5/thumbnails/4.jpg)
Why is this source so awesome?
• It is a binary that is both well-‐separated (1”5) and relatively tight (3.1 AU, P ≈ 20-‐40 yr)
• It is a flux reversal binary straddling the L dwarf/T dwarf transition
• It is highly variable in the optical
![Page 5: Luhman’16AB · Wavelength (!m) 0.6 0.8 1.0 1.2 1.4 1.6 1.8 2.0 Absolute F (10 h-17 erg/cm 2 /s/! m) 1.15 1.20 1.25 1.30 1.35 Wavelength (!m) Normalized Flux (F) h QP QP NaP H 2O](https://reader036.vdocuments.us/reader036/viewer/2022071017/5fd070a723f32170701a9535/html5/thumbnails/5.jpg)
Easy spectroscopic follow-‐up Resolved optical (Kniazev et al. 2013) and near-‐infrared (Burgasser et al. 2013) spectroscopy and photometry has been published,
Classified L7.5-‐L8 + T0-‐T0.5 optical & NIR
![Page 6: Luhman’16AB · Wavelength (!m) 0.6 0.8 1.0 1.2 1.4 1.6 1.8 2.0 Absolute F (10 h-17 erg/cm 2 /s/! m) 1.15 1.20 1.25 1.30 1.35 Wavelength (!m) Normalized Flux (F) h QP QP NaP H 2O](https://reader036.vdocuments.us/reader036/viewer/2022071017/5fd070a723f32170701a9535/html5/thumbnails/6.jpg)
Why is this source so awesome?
• It is a binary that is both well-‐separated (1”5) and relatively tight (3.1 AU, P ≈ 20-‐40 yr)
• It is a flux reversal binary straddling the L dwarf/T dwarf transition
• It is highly variable in the optical
![Page 7: Luhman’16AB · Wavelength (!m) 0.6 0.8 1.0 1.2 1.4 1.6 1.8 2.0 Absolute F (10 h-17 erg/cm 2 /s/! m) 1.15 1.20 1.25 1.30 1.35 Wavelength (!m) Normalized Flux (F) h QP QP NaP H 2O](https://reader036.vdocuments.us/reader036/viewer/2022071017/5fd070a723f32170701a9535/html5/thumbnails/7.jpg)
cf. SDSS 1534+1615AB (Liu et al. 2006) 2MASS 1404-‐3159AB (Looper et al. 2008) spectral binary candidates (Burgasser et al. 2010; Geiβler et al. 2011; Day-‐Jones et al. 2013)
Burgasser et al. (2013) also Kniazev et al. (2013)
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A late bloomer?
Luhman 16A & B are both red and underluminous @ J for their spectral types; young and/or cloudy? (cf. Looper et al. 2008)
Burgasser et al. (2013)
L7-‐L8 T0-‐T1
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Why is this source so awesome?
• It is a binary that is both well-‐separated (1”5) and relatively tight (3.1 AU, P ≈ 20-‐40 yr)
• It is a flux reversal binary straddling the L dwarf/T dwarf transition
• It is highly variable in the optical
![Page 10: Luhman’16AB · Wavelength (!m) 0.6 0.8 1.0 1.2 1.4 1.6 1.8 2.0 Absolute F (10 h-17 erg/cm 2 /s/! m) 1.15 1.20 1.25 1.30 1.35 Wavelength (!m) Normalized Flux (F) h QP QP NaP H 2O](https://reader036.vdocuments.us/reader036/viewer/2022071017/5fd070a723f32170701a9535/html5/thumbnails/10.jpg)
ESO/TRAPPIST
Michael Gillon
Gillon et al. (2013) 4.87±0.01 hr binary period variability appears to originate from T dwarf
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ATCA (5/2)
Keck/NIRSPEC IRTF/SpeX
IRTF/CSHELL
ESO/TRAPPIST Magellan/FIRE Magellan/MagE DuPont/Retrocam CTIO/Andicam CTIO/Las Cumbres
SAAO/ Las Cumbres
2013 April 22-‐28 Monitoring Campaign
NIR & Optical imaging and spectroscopy + radio interferometry Goals: characterize panchromatic variability, measure radial &
rotational velocities, search for magnetic emission
![Page 12: Luhman’16AB · Wavelength (!m) 0.6 0.8 1.0 1.2 1.4 1.6 1.8 2.0 Absolute F (10 h-17 erg/cm 2 /s/! m) 1.15 1.20 1.25 1.30 1.35 Wavelength (!m) Normalized Flux (F) h QP QP NaP H 2O](https://reader036.vdocuments.us/reader036/viewer/2022071017/5fd070a723f32170701a9535/html5/thumbnails/12.jpg)
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• ESO TRAPPIST
– optical variability: published (Gillon et al. 2013) • LCO/Retrocam + CTIO/Andicam + NTT/SofI
– optical and NIR variability: analysis underway (Radigan & Faherty) • Las Cumbres Chile + South Africa
– semi-‐continuous monitoring: analysis underway (Street) • Magellan/FIRE: NIR resolved moderate resolution (multi-‐epoch)
– improved RV & ΔRV and association membership: analysis complete (Faherty) – spectral variability: analysis underway (Faherty)
• Magellan/MagE: Optical resolved moderate resolution (multi-‐epoch) – spectral variability incl. Hα & Li I: analysis underway (Beletsky & Faherty)
• IRTF/SpeX: NIR resolved spectral monitoring
– component classification: submitted (Burgasser et al. 2013) – spectral variability: analysis underway (Burgasser)
• IRTF/CSHELL: NIR resolved high resolution – v sin i & ΔRV: analysis underway (Plavchan)
• Australian Telescope Compact Array – search for radio emission: analysis underway (Osten)
2013 April 22-‐28 Monitoring Campaign
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SOFI/NTT monitoring • Apr 27 2013 (J. Radigan)
• Non-ideal conditions (2” seeing) – combined light photometry
• J and K alternating
• fastPhot mode: variable “shade” pattern frame to frame currently limiting data reduction
achromatic trends
color variation
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Magellan/FIRE
0.8 1.0 1.2
Nor
mal
ized
Flu
x (F
)
1.4 1.6 1.8Wavelength (!m)
Luhman16A + L8 Standard
Luhman16B + T0 Standard
2.0 2.2 2.4
Faherty et al. (in prep)
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Faherty et al. (in prep)
Magellan/FIRE
0.8 1.0 1.2
Nor
mal
ized
Flu
x (F
)
1.4 1.6 1.8Wavelength (!m)
Luhman16A + L8 Standard
Luhman16B + T0 Standard
2.0 2.2 2.4
0.95 1.00 1.05 1.10Wavelength (!m)
Nor
mal
ized
Flu
x (F
)
FeH
FeH
CH4+H20
Luhman 16A
Luhman 16B
2.00 2.05 2.10 2.15 2.20 2.25 2.30 2.35Wavelength (!m)
Norm
alize
d Fl
ux (F
) CO
CH4
CIA H2
Luhman 16A
Luhman 16B
1.15 1.20 1.25 1.30 1.35Wavelength (!m)
Norm
alize
d Fl
ux (F
)
Na
H2OFeH
CH4
1.45 1.50 1.55 1.60 1.65 1.70 1.75Wavelength (!m)
Nor
mal
ized
Flu
x (F
)
FeHCH4
Luhman 16A
Luhman 16B
![Page 17: Luhman’16AB · Wavelength (!m) 0.6 0.8 1.0 1.2 1.4 1.6 1.8 2.0 Absolute F (10 h-17 erg/cm 2 /s/! m) 1.15 1.20 1.25 1.30 1.35 Wavelength (!m) Normalized Flux (F) h QP QP NaP H 2O](https://reader036.vdocuments.us/reader036/viewer/2022071017/5fd070a723f32170701a9535/html5/thumbnails/17.jpg)
Not an Argus member
1.242 1.245 1.248 1.251 1.254Wavelength (!m)
Norm
alize
d Fl
ux (F
)
Luhman 16A
Luhman 16B
2M1632 (L8 top)SD0151 (T1 bottom)
K I lines are strong, inconsistent with low surface gravity (Faherty et al. in prep)
With RV, kinematics are inconsistent with membership in any known moving group (Kniazev et al. 2013)
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1.240 1.245 1.250 1.255Wavelength (!m)
0.4
0.6
0.8
1.0
1.2
Nor
mal
ized
F
1.15 1.20 1.25 1.30 1.35Wavelength (!m)
No
rmal
ized
Flux
(F)
Na
H2OFeH
CH4
K I lines: Teff and clouds
Luhman 16A Luhman 16B
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1.240 1.245 1.250 1.255Wavelength (!m)
0.4
0.6
0.8
1.0
1.2
Nor
mal
ized
F
1.15 1.20 1.25 1.30 1.35Wavelength (!m)
No
rmal
ized
Flux
(F)
Na
H2OFeH
CH4
K I lines: Teff and clouds
Luhman 16A Luhman 16B
Burgasser et al. (2002); McGovern et al. (2004)
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1.240 1.245 1.250 1.255Wavelength (!m)
0.6
0.8
1.0
1.2
1.4
1.6
1.8
2.0
Abso
lute
F (1
0-17 e
rg/c
m2 /s
/!m
)1.15 1.20 1.25 1.30 1.35Wavelength (!m)
No
rmal
ized
Flux
(F)
Na
H2OFeH
CH4
K I lines: Teff and clouds
J-‐band continuum is dictated by cloud grain scattering
Luhman 16A Luhman 16B
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1.165 1.170 1.175 1.180Wavelength (!m)
0.4
0.6
0.8
1.0
1.2
1.4
Nor
mal
ized
F
1.15 1.20 1.25 1.30 1.35Wavelength (!m)
No
rmal
ized
Flux
(F)
Na
H2OFeH
CH4
K I lines: Teff and clouds
Luhman 16A Luhman 16B
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1.165 1.170 1.175 1.180Wavelength (!m)
0.4
0.6
0.8
1.0
1.2
1.4
1.6
Abso
lute
F (1
0-17 e
rg/c
m2 /s
/!m
)1.15 1.20 1.25 1.30 1.35Wavelength (!m)
No
rmal
ized
Flux
(F)
Na
H2OFeH
CH4
K I lines: Teff and clouds
1.17 µm continuum is dominated by H2O and CH4 opacity
Luhman 16A Luhman 16B
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1.240 1.245 1.250 1.255Wavelength (!m)
0.6
0.8
1.0
1.2
1.4
1.6
1.8
2.0
Abso
lute
F (1
0-17 e
rg/c
m2 /s
/!m
)
1.165 1.170 1.175 1.180Wavelength (!m)
0.4
0.6
0.8
1.0
1.2
1.4
1.6
Abso
lute
F (1
0-17 e
rg/c
m2 /s
/!m
)
1.15 1.20 1.25 1.30 1.35Wavelength (!m)
No
rmal
ized
Flux
(F)
Na
H2OFeH
CH4
K I lines: Teff and clouds
Luhman 16A Luhman 16B
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1.160 1.165 1.170 1.175 1.180 1.185Wavelength (µm)
1700
1600
1500
1400
1300
1200
1100
Brig
htne
ss T
empe
ratu
re (K
)
1.235 1.240 1.245 1.250 1.255 1.260Wavelength (µm)
1700
1600
1500
1400
1300
1200
1100
Brig
htne
ss T
empe
ratu
re (K
)
1.15 1.20 1.25 1.30 1.35Wavelength (!m)
No
rmal
ized
Flux
(F)
Na
H2OFeH
CH4
K I lines: Teff and clouds
Luhman 16A Luhman 16B
ΔT = 100 K
shallow
deep
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SpeX Spectroscopic Monitoring
Data
Model
Residuals
“Spectroscopic monitoring is a black art” -‐ anonymous
Luhman 16AB was monitored for 45 minutes with IRTF/SpeX during a downturn in TRAPPIST photometry NB: 1.2”-‐1.5” seeing, airmass = 3.4-‐3.5
![Page 26: Luhman’16AB · Wavelength (!m) 0.6 0.8 1.0 1.2 1.4 1.6 1.8 2.0 Absolute F (10 h-17 erg/cm 2 /s/! m) 1.15 1.20 1.25 1.30 1.35 Wavelength (!m) Normalized Flux (F) h QP QP NaP H 2O](https://reader036.vdocuments.us/reader036/viewer/2022071017/5fd070a723f32170701a9535/html5/thumbnails/26.jpg)
Unambiguous Flux Reversal
0 10 20 30 40Pixels
0.0
0.2
0.4
0.6
0.8
1.0
1.2
Profile
J K
1.0 1.2 1.4 1.6 1.8 2.0 2.2Wavelength (!m)
0
2•10-15
4•10-15
6•10-15
8•10-15
1•10-14
Appa
rent
F
Luhman 16A Luhman 16B
![Page 27: Luhman’16AB · Wavelength (!m) 0.6 0.8 1.0 1.2 1.4 1.6 1.8 2.0 Absolute F (10 h-17 erg/cm 2 /s/! m) 1.15 1.20 1.25 1.30 1.35 Wavelength (!m) Normalized Flux (F) h QP QP NaP H 2O](https://reader036.vdocuments.us/reader036/viewer/2022071017/5fd070a723f32170701a9535/html5/thumbnails/27.jpg)
h4p://youtu.be/DIJx0flF6uc
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6.2 6.4 6.6UT Time on 26 April 2013 (hours)
0.80
0.85
0.90
0.95
1.00
1.05
1.10
1.15R
elat
ive
Flux
(B/A
) TRAPPIST light curve
Continuum Flux + 0.1
Band Flux - 0.1
Relative fluxes (B/A) show similar decline as broadband photometry
No difference between continuum and band fluxes
Consistent with a decline in B’s brightness, but better calibration is required
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high resolution optical spectroscopy with
MIKE to measure ΔRV
v sin i measurements with CSHELL + 13CH4 gas cell (Anglada-‐Escudé et al. 2012)
multi-‐color continuous
photometry with the Las Cumbres
network
most stringent radio and Hα flux constraints for brown dwarfs
improved NIR spectral monitoring with HST/
WFC3 (cf. Apai et al. 2013)
tighter parallax and
proper motion
measures
let’s test those cloudy
atmosphere models! (cf. Leggett
et al. 2008)
MIR variability
with Spitzer/IRAC (cf. Heinze
et al. 2013)
orbit constraints, masses soon(astro + RV)