RESOLVE & ECO: the REsolved Spectroscopy of a Local …caziegle/RESOLVEtalk.pdf · RESOLVE & ECO:...
Transcript of RESOLVE & ECO: the REsolved Spectroscopy of a Local …caziegle/RESOLVEtalk.pdf · RESOLVE & ECO:...
RESOLVE & ECO:the REsolved Spectroscopy of a Local VolumE Survey
and its Environmental COntext Catalog
Sheila Kannappan
UNC Chapel Hill
• volume-limited, unusually complete census of dynamical, stellar, and gas mass, plus star formation/merging/chemical evolution, from dwarf galaxy to cluster scales
• >50,000 cubic Mpc
• >1500 galaxies
• baryonic mass limit ~109 Msun
• 1” = 0.3-0.5 kpc
• volume-limited design enables robust metrics of environment
• new 21cm data & 3D optical spectroscopy + superior reprocessed photometry
two equatorial stripscz=4500-7000 km/s525 sq deg A-sem187.5 sq deg B-sem
REsolved Spectroscopy Of a Local VolumE
RESOLVE-A
RESOLVE-B
RESOLVE-B:
Stripe 82: extra deep; hyper-complete – czcampaign for galaxies lost by SDSS (dwarfs, pairs, shredded spirals)
Find empirical completeness corrections larger than predicted by Blanton et al. (Eckert+ 2016).
ECO: “Environmental COntextcatalog” (~10x larger, all same pipelines for stellar mass, envt; Moffett+ 2015)
Contains RESOLVE-A; enables calibration of cosmic variance.
More complete than SDSS.
Cosmic Variance and Completeness
original SDSS limit
Why go down to 109 Msun across environments?
baryonic physics should change at key halo/galaxy mass scales
“cold” accretion shuts down from the inside out over a range in halo mass (e.g., Dekel & Birnboim 2005)
threshold~1011.4 Msun
bimodality~1012.1 Msun
shutdown~1013.3 Msun
Rvir
0.1Rvir
Rvir
0.1Rvir
Eckert et al. 20
15blog group halo mass from abundance matchinglo
g g
alax
y m
ass
(ste
llar
or
bar
yon
ic)
halo mass scales translate to (central) galaxy mass scales
Why go down to 109 Msun across environments?
baryonic physics should change at key halo/galaxy mass scales
“cold” accretion shuts down from the inside out over a range in halo mass (e.g., Dekel & Birnboim 2005)
threshold~1011.4 Msun
bimodality~1012.1 Msun
shutdown~1013.3 Msun
Rvir
0.1Rvir
Rvir
0.1Rvir
Eckert et al. 20
15blog group halo mass from abundance matchinglo
g g
alax
y m
ass
(ste
llar
or
bar
yon
ic)
halo mass scales translate to (central) galaxy mass scales
These scales are associated with missing baryons, galaxy SF/gas/metallicity transitions (Dalcanton, Kannappan), deficits in
the dwarf inventory (e.g. “too big to fail” in the field; Papastergis+ 2015),
and also group formation. Need complete mass census.
Rvir
0.1Rvir
Rvir
0.1Rvir
Why go down to 109 Msun across environments?
baryonic physics should change at key halo/galaxy mass scales
These scales are associated with missing baryons, galaxy SF/gas/metallicity transitions (Dalcanton, Kannappan), deficits in
the dwarf inventory (e.g. “too big to fail” in the field; Papastergis+ 2015),
and also group formation. Need complete mass census.
structure halo mass
thresh
old
scale
galaxies groups
Vobs
McG
aug
h+
2010in
teg
rate
d s
tru
ctu
re b
aryo
nic
mas
s
threshold~1011.4 Msun
bimodality~1012.1 Msun
shutdown~1013.3 Msun
Key scales imprinted on RESOLVE HI census(>95% complete, Stark et al. 2016)
ga
s-r
ich
ne
ss th
resh
old
bim
od
alit
y
sh
utd
ow
n
up
dat
e o
f K
ann
app
an+
20
13
crucial survey design features:• complete to well below key gas content transition scales• HI data fractional-mass limited (5-10% Mstellar upper limits)
inco
mp
lete
≡ stellar + HI gas
Improvements (not standard!):
• Blanton sky subtraction
• gri coadds define ellipses
• color gradients allowed
• flux extrapolation 3 ways
brighter, bluer, larger galaxies with more real scatter in color
Eckert+ 2015a
(Exciting!) reprocessed photometry(Eckert+ 2015 for RESOLVE; Moffett+ 2015 for ECO)
•
• broad
• blue
• red
SOAR
Gemini
~few arcsec
~12”x 100”SALT
~few arcmin
custom image slicer
RESOLVE’s 3D Optical Spectroscopy Census(dynamics, metallicity, star formation history, AGN…)
size (arcsec)
incl
inat
ion
Q: what’s missing here?
SIFS, AAT
unfinished red setup
Results: Old, New, Borrowed, Blue
Identification of NGC4546-UCD 1 using SOAR redshift data –
smoking gun formation of an ultra compact dwarf by stripping
(Norris & Kannappan 2011; pilot for AIMSS)
“kinematic
memory” of
mass before
stripping
standard
track for
unstripped
galaxies
two tracks (as in AIMSS, Norris+ 2014) with “crossover” objects (E. Snyder MA thesis 2016)
RESOLVE cEs
dEs
M32 Huxor’s cE
Results: Old, New, Borrowed, Blue
envelope-dominated core-dominated
census of compact core galaxies in RESOLVE
SOAR
Gemini GMOS-IFU #11, “crossover” cE
SOAR 1” slit – #13, ambiguous cE
a little IFU can go a long way…
Results: Old, New, Borrowed, Blue
“kinematic
memory” of
mass before
stripping
standard
track for
unstripped
galaxies
two tracks (as in AIMSS, Norris+ 2014) with “crossover” objects (E. Snyder MA thesis 2016)
RESOLVE cEs
dEs
M32 Huxor’s cE
envelope-dominated core-dominated
census of compact core galaxies in RESOLVE
Results: Old, New, Borrowed, Blue
Eckert et al. 2016
nascent groupisolated dwarf
large group
cluster
Full BMF hides complex envt-dependent structure!
Results: Old, New, Borrowed, Blue
Eckert et al. 2016
Full BMF hides complex envt-dependent structure!
10 11 12 13 14 15halo mass (logMsun)
100
101
102
103
104
105
106
nu
mb
er
of
ha
los/b
in
Bolshoi simulationprediction
nascent groupisolated dwarf
large group
cluster
Results: Old, New, Borrowed, Blue
Eckert et al. 2016
Full BMF hides complex envt-dependent structure!
satellites!satellite stripping?
10 11 12 13 14 15halo mass (logMsun)
100
101
102
103
104
105
106
nu
mb
er
of
ha
los/b
in
Bolshoi simulationprediction
Results: Old, New, Borrowed, Blue
double nucleus found with SAM FP
Identification of blue nuggets at redshift zero: “prolate” starbursts analogous to first high-redshift galaxies; question
whether formed by mergers or converging gas streams
Found two; six more candidates pending confirmation this spring (more SAM FP data + Gemini Fast Turnaround program led by undergrad!)
minor axis rotation seen with GMOS confirmed
with SOAR SAM FP
DECaLS image
Alumni of the RESOLVE/ECO team
• Kathleen Eckert, PhD 2016 (now cosmology postdoc at Penn)• galaxy and group mass functions: probing dark matter halo physics• metrics of stellar, gas, and dynamical mass for galaxies and groups• optical instrumentation
• Elaine Snyder, MA 2016 (now research & instrument analyst at STScI)• compact core galaxies: probing stripped nuclei vs. tiny mergers• numerical simulation of tidal stripping (led by REU student)
• David Stark, PhD 2015 (now prize postdoc at Kavli IPMU in Tokyo)• atomic gas (HI 21cm line) census and environment/halo mass
drivers of galaxy gas content• search for star formation in Milky Way high velocity cloud• galaxy fueling: atomic-to-molecular gas conversion & fresh gas accretion
• Amanda Moffett, PhD 2013 (now prize postdoc at Vanderbilt + SAMSI affiliate)• stellar disk regrowth around merger remnants: XUV disks and blue E/S0s• environment/halo mass drivers of galaxy disk growth• optical instrumentation
• Mark Norris, postdoc 2008-2012 (now faculty at UC Lancashire)• S0 galaxy dynamics in RESOLVE (now led by A. Moffett)• compact stellar systems and the AIMSS survey