Sandy Faber (Scientific highlights of the DEEP2 and AEGIS):
DEEP2: 53000 spectra, 4 fields 3 square degrees. ~39000 spectra with good quality. AEGIS:
Quenching of galaxies:
Bell et al. (2004): COMBO-17 finds that the red galaxy population grew by a factor of 2 in number density since z~1. Red sequence is forming form the blue cloud.
External models:
Massive halo quenching: truncation of cold flows and conversion of cold gas to hot halos in haloes above 10^12 Msun.
Internal models:
stellar feedback, AGNs.
secular evolution, disk instability
quenching is gradual, and it first starts in dense environments. Massive red sequence quench first.
Conroy Wechsler and Croton:
U-B vs sersic index Z shape plot.Perhaps internal processes are at shape, otherwise why will the internal structure predict the color (red or blue).
Stellar feedback driven by mergers does not work because it can be fast.
Look at Noeske (2007).
SSFR vs M* Salim et al.
AGNs are not related to mergers somehow.
Disk fading!?
Garth Illingworth: Growth of galaxies between z~4-10
reionization, fast galaxy growth.
Finding high z galaxies: Lyman break technique. contamination!?
Bouwens et al. nature paper z~10 galaxy.
Slope at the faint end very steep, so may be important for reionization.
What is this beta?
Guzman: Size evolution
There is still debate about the size velocity dispersion relation at high z. van Dokkum et al. and Trujillo et al.
Fading + minor merger can show how galaxies evolve in the fundamental plane, faber jackson, and M-Re to evolve from z~1 to z~0.
Gallego: SFGs at z~0.8 with Halpha
Quenching mass is an order of magnitude higher at high redshift.
How to get quenching mass? doubling time from SSFR and compare it to quenching time which is assumed to be 3 times the Hubble time ?! Villar et al. (2008,2011), and how does one get the halo mass (?!)
Lowenthal: LCBGS are they counterparts of lyman break galaxies?
From HST imaging, no disky structure, just irregulars: both at high and low redshift.
Similar to Elmegreen;s high z galaxies.
morphologies similar in NIR-opt and UV.
Windhorst: Panchromatic survey
Wyithe et al. 2011 (Nature paper) Lensing might be causing the luminosity functions to be wrong at high z.
Szalay:
BEKS 1990: 128 hinv Mpc.
Along the line of sight the signal to noise ratio is higher for the BAO.
Bershady: Galaxy disks are submaximal
Use statisitical measure of the height from edge on disk galaxies, and use the epicyclic velocities of stars in face on galaxies, out of the plane of the galaxy.
Raja Guhathakarta:
Bruzual: Problem in SPS
Fall:
The mass function of star clusters shows a power law with slope 2 in many many galaxies. As star clusters age, they get disrupted, but they maintain the mass function slope. There is also a distribution of ages for the clusters which is uniform in many galaxies.
Mass removal processes: stellar activity to unbind the clusters. stellar mass loss, tidal disturbances by passage of molecular clouds.
Internal relaxation in older clusters.
No AGN merger connection from CANDELS data.
Seems disk instabilities cannot be the reason.
Secular processes/ minor mergers with small time delays are ok
David Koo
MgII outflows with SDSS?
Signature of inflows seen in some red sequence galaxies.
Avishai:
Streams come along a plane. On average 5 streams.
One stream dominates the angular momentum fed into the disk. The disk is very very weakly aligned with the angular momentum of the stream at Rvir. In the inner parts the angular momentum do align very well. It is within the interaction region, that ht estreams break up exchange angular momenta and change directions.
Toomre < 1 instability.
Q=sigma omega/(GSigma)
AGN due to inward radial movement due to disk instabilities.
Marcello:
Evolution of the gas density, stellar velocity dispersion as a function of redshift for disc galaxies. Assuming marginally unstable disks are maintained all the time: physically expected: some feedback loop, need to think about it. Unless the velocity dispersion of the gas goes down to a value ~ to the sound speed.
Romeel Dave
How does the hot gaseous winds inhibit cold flows?
Photoionization, AGN, gravity and winds prevent
SFR, fgas, Metallicity as a function of redshift.
Fumagilli
Cold streams are lyman limit systems seen in quasar spectra.
Behroozi:
Bayesian analysis to include both the stellar mass functions and the SFR density(z) . Incompleteness (z) completely arbitrary function
Paul Oesch: HUDF
Dusan Keres: AREPO vs GADGET
more extended, regular disks. The extended disks are easier to strip and this increases mixing with hot halo, the star formation increases due to the efficient cooling of the hot halo.
Spectral fluctuations in HST pixels.
James Bullock:
Galactic conformity raises its hood again. This needs to be killed soon, else it will create news again.
Michael Boylan Kolchin:
Matching the luminosity function of the milky way satellites is ok, but getting the densities correct is a problem. Most likely related to baryonic effects changing the properties of the dark mater in subhaloes.
Chung-Pei Ma:
Massive black holes, using IFU, get the stellar kinematics and use Schwarzschild modeling to get the black hole mass, have M/L ratio as parameter, dark matter halo, and the black hole mass. Question about how to measure the bulge dispersion. Can M/L ratio give some constraints on the IMF? Check on how the kinematics are modeled.
Things to be improved:
Fitting of lines: Black hole mass-bulge mass relation, Lx Tvir relation and so on.
Group catalog, proper environment study. Hopefully the previous large scale environment !? Although this is doubtful...
HOD modelling of the Lyman break galaxies. Incompleteness-redshift relations, may not be the rightest way, is it?
High redshift mass functions and how they compare to Tinker et al. Revision of the reionization estimates.
===========
Workshop on astro-informatics (2012)
Sandy Faber (Scientific highlights of the DEEP2 and AEGIS):
DEEP2: 53000 spectra, 4 fields 3 square degrees. ~39000 spectra with good quality. AEGIS:
Quenching of galaxies:
Bell et al. (2004): COMBO-17 finds that the red galaxy population grew by a factor of 2 in number density since z~1. Red sequence is forming form the blue cloud.
External models:
Massive halo quenching: truncation of cold flows and conversion of cold gas to hot halos in haloes above 10^12 Msun.
Internal models:
stellar feedback, AGNs.
secular evolution, disk instability
quenching is gradual, and it first starts in dense environments. Massive red sequence quench first.
Conroy Wechsler and Croton:
U-B vs sersic index Z shape plot.Perhaps internal processes are at shape, otherwise why will the internal structure predict the color (red or blue).
Stellar feedback driven by mergers does not work because it can be fast.
Look at Noeske (2007).
SSFR vs M* Salim et al.
AGNs are not related to mergers somehow.
Disk fading!?
Garth Illingworth: Growth of galaxies between z~4-10
reionization, fast galaxy growth.
Finding high z galaxies: Lyman break technique. contamination!?
Bouwens et al. nature paper z~10 galaxy.
Slope at the faint end very steep, so may be important for reionization.
What is this beta?
Guzman: Size evolution
There is still debate about the size velocity dispersion relation at high z. van Dokkum et al. and Trujillo et al.
Fading + minor merger can show how galaxies evolve in the fundamental plane, faber jackson, and M-Re to evolve from z~1 to z~0.
Gallego: SFGs at z~0.8 with Halpha
Quenching mass is an order of magnitude higher at high redshift.
How to get quenching mass? doubling time from SSFR and compare it to quenching time which is assumed to be 3 times the Hubble time ?! Villar et al. (2008,2011), and how does one get the halo mass (?!)
Lowenthal: LCBGS are they counterparts of lyman break galaxies?
From HST imaging, no disky structure, just irregulars: both at high and low redshift.
Similar to Elmegreen;s high z galaxies.
morphologies similar in NIR-opt and UV.
Windhorst: Panchromatic survey
Wyithe et al. 2011 (Nature paper) Lensing might be causing the luminosity functions to be wrong at high z.
Szalay:
BEKS 1990: 128 hinv Mpc.
Along the line of sight the signal to noise ratio is higher for the BAO.
Bershady: Galaxy disks are submaximal
Use statisitical measure of the height from edge on disk galaxies, and use the epicyclic velocities of stars in face on galaxies, out of the plane of the galaxy.
Raja Guhathakarta:
Bruzual: Problem in SPS
Fall:
The mass function of star clusters shows a power law with slope 2 in many many galaxies. As star clusters age, they get disrupted, but they maintain the mass function slope. There is also a distribution of ages for the clusters which is uniform in many galaxies.
Mass removal processes: stellar activity to unbind the clusters. stellar mass loss, tidal disturbances by passage of molecular clouds.
Internal relaxation in older clusters.
No AGN merger connection from CANDELS data.
Seems disk instabilities cannot be the reason.
Secular processes/ minor mergers with small time delays are ok
David Koo
MgII outflows with SDSS?
Signature of inflows seen in some red sequence galaxies.
Avishai:
Streams come along a plane. On average 5 streams.
One stream dominates the angular momentum fed into the disk. The disk is very very weakly aligned with the angular momentum of the stream at Rvir. In the inner parts the angular momentum do align very well. It is within the interaction region, that ht estreams break up exchange angular momenta and change directions.
Toomre < 1 instability.
Q=sigma omega/(GSigma)
AGN due to inward radial movement due to disk instabilities.
Marcello:
Evolution of the gas density, stellar velocity dispersion as a function of redshift for disc galaxies. Assuming marginally unstable disks are maintained all the time: physically expected: some feedback loop, need to think about it. Unless the velocity dispersion of the gas goes down to a value ~ to the sound speed.
Romeel Dave
How does the hot gaseous winds inhibit cold flows?
Photoionization, AGN, gravity and winds prevent
SFR, fgas, Metallicity as a function of redshift.
Fumagilli
Cold streams are lyman limit systems seen in quasar spectra.
Behroozi:
Bayesian analysis to include both the stellar mass functions and the SFR density(z) . Incompleteness (z) completely arbitrary function
Paul Oesch: HUDF
Dusan Keres: AREPO vs GADGET
more extended, regular disks. The extended disks are easier to strip and this increases mixing with hot halo, the star formation increases due to the efficient cooling of the hot halo.
Spectral fluctuations in HST pixels.
James Bullock:
Galactic conformity raises its hood again. This needs to be killed soon, else it will create news again.
Michael Boylan Kolchin:
Matching the luminosity function of the milky way satellites is ok, but getting the densities correct is a problem. Most likely related to baryonic effects changing the properties of the dark mater in subhaloes.
Chung-Pei Ma:
Massive black holes, using IFU, get the stellar kinematics and use Schwarzschild modeling to get the black hole mass, have M/L ratio as parameter, dark matter halo, and the black hole mass. Question about how to measure the bulge dispersion. Can M/L ratio give some constraints on the IMF? Check on how the kinematics are modeled.
Things to be improved:
Fitting of lines: Black hole mass-bulge mass relation, Lx Tvir relation and so on.
Group catalog, proper environment study. Hopefully the previous large scale environment !? Although this is doubtful...
HOD modelling of the Lyman break galaxies. Incompleteness-redshift relations, may not be the rightest way, is it?
High redshift mass functions and how they compare to Tinker et al. Revision of the reionization estimates.