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

Data Releases

http://resolve.astro.unc.edu

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

Summary of survey design

• Key advantages of RESOLVE & ECO:

• Additional benefits of RESOLVE:

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

preliminary

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

Why isn’t SOAR the centerpiece of RESOLVE publications to date?