Galaxy Evolution: Current Surveys and InstrumentationOuter disk stars, cold gas dwarfs & galactic...
Transcript of Galaxy Evolution: Current Surveys and InstrumentationOuter disk stars, cold gas dwarfs & galactic...
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Galaxy Evolution: Current Surveys and Instrumentation
Matthew BershadyUniversity of Wisconsin-Madison
Credits:DiskMass Survey teamSDSS-IV/MaNGA team
N3953 N891
SDSS gri WHIRC JHK
KMOS z=0.8 Main Sequence (Stott+14)
HSTMW archetypes
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Outline
⢠Theme:
â Is the MW a typical spiral galaxy?
⢠State of the Art Instrumentation
â Monoliths, Megaliths & MOS
⢠Key topics
â Heating and cooling of disks
â dwarfs and the galactic periphery
â
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Licquia & Newman (2014)
MW
6918
3701
81964256
4368
3997
4380
7917
4458
BC03
4256
6918
37018196
43683997
4458
4380
7917
MW
Bershady+2015DMS: Bershady+10, Martinsson+2013
I. Is the Milky Way a typical galaxy?
DiskMass Survey
M/L and star-formation: MW and the DiskMass Survey
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Outstanding issues
⢠The Milky Way appears to have a maximal disk and a very small size for its rotation speed.
⢠DiskMass Survey spirals have submaximal disks.
Do we really live in an unusual galaxy? âŚor are different vantage points leading to
observational bias? e.g., mass vs light weightingâŚ
Courteau et al. 2007
Bovy+14cf Iocco+15
Bershady+11Martinsson+13
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II. State of the Art is IFS
⢠The future just arrivedâ MUSE â VLT 8mâ VIRUS â HET 10mâ MOS
⢠KMOS â VLT 8m⢠SAMI â AAT 3.9m⢠MaNGA â Sloan 2.5m
⢠Common themes:â Large AWinstrument multiplexâ Few have large specific grasp AdW
â object multiplex:different solutions⢠KMOS and MUSE: slicers⢠VIRUS, SAMI, MaNGA: fibers
â instrument multiplex:cost-driven⢠Economies of scale⢠Limited camera field
Wide-field
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MUSE
⢠Science goalsâ Detailed study of high-redshift galaxies,
structure formation, discovery.
⢠Technical approachâ Replicate 24 modest-resolution
spectrographs fed with advanced (catadioptric) images slicers.
â Premium on image quality / information.â Ground-layer AO (GLAO) assisted.
⢠Instrument capabilitiesâ VLT 8mâ Two scales:
⢠1 arcmin2 FoV, (0.04 arcsec2 elements)⢠56 arcsec2 FoV, (6.3x10-3 arcsec2)
â integrally sampledâ 0.465-0.93 nm range (one shot)â ~2000 spectral elements (R~3000)â e ~ 0.24
Bacon et al. â04
AMAZING
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MUSE: great contributions at low-z
UGC 463
stel
lar
[OII
I]V
-fie
ld
PPaK MUSE
Martinsson+13
MUSE
PPK
Martinsson & Brinchmann+15
1h5h
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But thereâs a real need for better spectral resolution:MUSE canât kinematically resolve gas dispersions in normal disks
SparsePak
MUSE
MUSE: great contributions at low-z
Ha
MUSE
Ha + Hb
1 x 15min0.â6x0.â6 spaxels
1h Ha
10h MgI4.â7 spaxels
Martinsson & Brinchmann+15 Westfall+11
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VIRUS
⢠Science goalsâ Measure BAO from Lya-eâs at
1.8<z<3.7: HETDEX
⢠Technical approachâ Replicate 150, small, cheap, low
resolution bare-fiber fed spectrographs
⢠Instrument capabilitiesâ HET 10m + new corrector
â 16.5â field, sparsely sampled
â 75 IFUs, 16.5 arcmin2 coverage
â 33600 fibers (1.5â diam.)
â 350-550 nm range (one shot)
â 410 spectral elements (R~700)
â e ~ 0.15
50â448fibers
Hill+12a,b
16.5â
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KMOS
⢠Science goalsâ Investigate physical properties driving galaxy
formation/evolution; measure comoving star-formation rate.
⢠Technical approachâ Multi-object image slicer feeding cryogenic
spectrographs (3).
⢠Instrument capabilitiesâ VLT 8m
â 24 MOS probes, 2.8x2.8 arcsec each, sampled at 0.2 arcsec (14 slices)
â 4704 spatial elements total (188 arcsec2)
â 7.2 arcmin diameter patrol field
â 0.8-2.5 mm range
â 1000 spectral elements (R~3600)
â e = 0.3 * telescope * atmosphere
Sharples+12
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CALIFA, SAMI and MaNGA
⢠Science goalsâ Dissect nearby galaxy population to determine
dynamics and composition physical properties driving galaxy formation/evolution;
⢠Technical approachâ Multi-object fiber IFUs feeding dual-beam
spectrographs.
⢠Instrument capabilities15â1.6â fibers
4 x 61 fibers2 x 19-fibers
2 x 91-fibers
5 x 127-fibers
4 x 37-fibers
2â fibers12â-32â diameters
CALIFA SAMI MaNGA
DTEL CA 3.5m AAO 3.9m SDSS 2.5m
Patrol FoV 1 deg 3 deg
# IFU 1 13 17
# fibers 382 819 1423
Dfiber 2.7â 1.6â 2.0â
IFU FoV 70â 15 12-32â
spectrograph PMAS AAOmega BOSS
Îť coverage (nm) 380-730 370-570, 625-735
350-1050
R=Îť/dÎť 1500,1100 1730,4500 1400-2700
Efficiency, e 0.13 0.09,0.14 0.30
13 x 61 fibers
SAMI: Croom+12
MaNGA: Bundy+15
CALIFA:Sanchez+12PPK: Verheijen+â04, Kelz+â06PMAS: Roth+â05
70â
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Metrics
This doesnât do justice to the spectral resolution and simulataneouscoverage (spectral power) of WEAVE
Hill 2014
MaNGA / SDSS-IVo Sloan 2.5m telescope o 3 deg FoVo 2 x dual-channel spectrographso 17 IFUso 1423 fiberso 2â diameterso 12â-32â IFU FoVo R=2000, 360-1050nm
See also: Weijmans â MaNGAFalcon-Barroso, Delgado â CALIFACroom - SAMI
Bundy+2015 (MaNGA PI)
ISM
stellar
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Telescope, diameter WHT, 4.2m
Field of view 2Âş
MOS fibers ~1000 x 1.3â diameter
Number of small
IFUs, size
20, 10âx14â (1.3â
spaxels)
LIFU size1.5âx1.2â (2.6â
spaxels)
Low-resolution modeR = 4300â7200
366â984 nm
High-resolution mode
R=18560â21375
404â465, (473â545)
595â685 nm
WEAVE / IFUs and key parameters
14â
11â
20 mini-IFUs coexist with MOS
NB: 32m fiber run â UV attenuation
20 x
Dalton+â12 (credit also: S. Trager)
Verheijen Ă la PPAK
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Spectral resolution⢠At dl/l = 9000 (33 km s-1
FWHM) with galaxy internal velocity spread of 150 km s-1 (5:1) sky lines can be completely removed.
⢠Lower resolution significantly degrades spectral data.
dl/l = 35000
(Osterbrock+96)
Sky resolved at:dl/l = 2300
dl/l = 9000
.5
1
no mask
.5
1
contin
uumâ
norm
aliz
ed f
lux
mask
sky
840 860 880
1
10
100
wavelength (nm)
Bershady+10
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Spectral resolution
dl/l =12000, 4800, 2400, 1200 s (km/s) = 11, 26, 53, 110
E, bulges
Inner disks
Mid-disk stars ~ ionized disk gas
Outer disk stars, cold gas dwarfs & galactic periphery
WEAVE MUSE
SAMICalifa
MaNGA
DiskMass ATLAS3D
2000 ADSauron
2020 AD
wavelength (nm)
normalized flux
501504
507510
513
.5 1
1.5
[OIII]
MgI
FeI,FeIITiI,TiII,NiICrI,CrII,TiOHeI,OII
MgI
FeI,FeIITiI,TiII,NiICrI,CrII,TiOHeIOII
wavelength (nm)
normalized flux
513516
519522
525
.5 1
1.5
MgIb
[NI]
MgI
FeI,FeIITiI,TiII,NiICrI,CrII,TiOHeI,OII
MgI
FeI,FeIITiI,TiII,NiICrI,CrII,TiOHeIOII
Best abundance information in dynamically cold systems if you have the spectral resolution.
s (km/s) 11 29 77
Bershady+10
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III. Key questions
Disk assembly: settling, heating or both?
⢠Why this question: â Go beyond distributions of integrated properties, e.g.,
galaxy mass-function, Ď(M,âŚ)
â Directly probe astrophysical processes of mass assembly with resolved maps of mass, kinematics, and composition for galaxy populations
â Couple to full chemo-dynamical phase-space for gas and stars uniquely accessed in MW
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Disk assembly: settling, heating or both?
1. The Milky Way as a Galaxy
2. The look-back record: distant galaxies
3. Breakthroughs very nearby: M31 & NGC 891
4. Statistical studies of low-z galaxies
5. Concluding challenges
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Disk assembly: settling, heating or both?
1. The Milky Way as a Galaxy⢠Historical debate on origin stellar disk heating
e.g., Spitzer & Schwarzchild+51, Weilenâ77, Ostrikerâ86, Binney+â00
⢠Thick disk controversy cf Gilmore & Reidâ83, Bovy+12; see also Brook+04, Forbes+12, Bird+13, Martig+14, Minhchev+13,14
⢠Data renaissance: RAVE (Steinmetz+06), SEGUE (Yanny+2009; SDSS-II), GALAH/HERMES (De Silva+15), APOGEE-1,2 (Majewski+15; SDSS-III,IV)
⢠Earth-quake in process: GAIA
SDSS: Du+03
Hipparcos: Binney+00
young old
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2. The look-back record: photometry(a) build-up of stellar mass with time and radius in MW-mass galaxies is smooth, inside out, with 90% assembled between 0.4 < z < 2.5
van Dokkum+13
log(M)~10.7
Disk assembly: settling, heating or both?
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2. The look-back record: kinematics(b) ionized gas disks appear to settle
with time
â DEEP - Kassin+07,12
â SINS - FĂśrster Schreiber+09
Bournaud+09
â KMOS - Wisnioski+15
VELOCITY FIELDS
Total Sellar Mass
SFR
z<1.2
z<3
Brook+04: Origins of thick disk as a relic of a more turbulent era.
Disk assembly: settling, heating or both?
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2. The look-back record: (c) settling must be a function of merger and SF history
DYNAMO: Green+13
Disk assembly: settling, heating or both?
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2. The look-back record: simulations⢠Heating and cooling/settling of gas disk imprinted on stars observed today⢠Establishes age-velocity-metallicity relations (e.g., Minchev+12,14; Martig+14a,b)⢠Relative roles of heating vs settling unclear: cf Bird+13, Martig+14a
⢠Disks form âinside out and upside downâ⢠Heating relatively unimportant after 1-2Gyr
Disk assembly: settling, heating or both?
Bird+13
settling
heatingsz
(km
/s)
Vro
t/
sz
Med
ian
z (
kpc)
Time (Gyr) Time (Gyr)
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2. The look-back record: simulations⢠Heating and cooling/settling of gas disk imprinted on stars observed today⢠Establishes age-velocity-metallicity relations (e.g., Minchev+12,14; Martig+14a,b)⢠Relative roles of heating vs settling unclear: cf Bird+13, Martig+14a
⢠Different merger histories (heating) is important
Disk assembly: settling, heating or both?
sz
(km
/s)
z 0 (k
pc)
sz
(km
/s)
z 0 (k
pc)
Age (Gyr)
Martig+14a
Radius (kpc) Radius (kpc)
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3. Very nearby: Resolved stellar kinematics in M31 ⢠age-velocity-metallicity relations not the same for two massive LG spirals
Dorman+15
Zage
Disk assembly: settling, heating or both?
M31
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⢠NGC 891 K-band vertical light profile well fit by
MW heating model and constant SFR for ~9-12
Gyr
Mouchine et al. 2010Subaru star counts
Schechtman-Rook et al. 2012c
observed
Disk assembly: settling, heating or both?
3. Very nearby: NGC 891 heating model
Bershady+15
Excess
light
above 1
kpc is 1-
2% of total
disk light
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The universe is logarithmic; why arenât our instruments?
Disk assembly: settling, heating or both?
3. Very nearby: variable pitch IFUs
Wood+12
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z(kpc)
wavelength (nm)
z ~ 2 kpc
NGC 891
1
400 1000600 800
Break-point: chronometer
Vertical gradients in spectrao ⌠ageo ⌠metallicity
2
0
R ~ 2,000, BC03
Disk assembly: settling, heating or both?
3. Very nearby: spectro-photometric chronometers
Sensitivity in blue
Break-point height and width measures heating time-scale & SFH Bershady+15
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height (kpc)0 1 2
AV
(mag
)Li
ght-
wei
ghte
d a
ge (
Gyr
)
5
3
1
0
12
8
4
Z = 0.5 Z sol
Disk assembly: settling, heating or both?
3. Very nearby: vertical population gradients
Pak observations
Eigenbrot+15
⢠Can be applied to large samples⢠NB: must account for different LOS depth w/height
NGC 891
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⢠Mapping Nearby Galaxies at APO⢠One of 3 surveys in SDSS-IV⢠IFU spectroscopy of 10,000 galaxies in 6 years⢠Cover 350 - 1050nm at resolution of 60 km/s⢠Sample all galaxy types and environments⢠Multiplex 17 IFUs at once
PI: Kevin Bundy
Disk assembly: settling, heating or both?
4. MaNGA: a statistical approach
MaNGABundy et al. 2015
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Projected tangential velocities (ârotation curvesâ) of gas and stars show Asymmetric Drift
Measuring stellar velocity dispersions with only velocities
Westfall+ 2014
Asymmetric drift (AD) depends on in-
plane Ď* (ĎR, ĎĎ), radial derivatives of
V and Ď, and shape of Ď-ellipsoid.
Epicycle approximation
AD
vR and vRvĎmoments of the collisionlessBoltzman equation
1. measure Vg, V*
2. infer Ď*
3. calibrate with DiskMass Survey
Disk assembly: settling, heating or both?
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4. MaNGA: Asymmetric Drift
7443-12702
7443-6102
7495-12703
stars gas7495-12704
7815-9101
7977-12703
stars gas
Disk assembly: settling, heating or both?
Bundy+15, Westfall+15
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Summary Charge to the Community
5. Challenges:
a) Measure stellar disk dynamics, ages, and abundances outside of the local group
o How: large-grasp IFUs with broad spectral coverage and high spectral resolution
b) Define the observational test distinguishing between disk settling (cooling) and stellar heating.
o Make this a well-posed problem.
Disk assembly: settling, heating or both?