Results are all preliminary andResults are all preliminary ...
Preliminary Lens Models for Massive Planck Clusters in the ...kerens/files/cerny_poster_2016.pdf ·...
1
Preliminary Lens Models for Massive Planck Clusters in the RELICS Survey Cerny, Catherine (University of Michigan); Sharon, Keren (University of Michigan); Coe, Dan (Space Telescope Science Institute [STSCI]); Jones, Christine (Smithsonian Institution Astrophysical Observatory); Czakon, Nicole (Academia Sinica, Institute of Astronomy and Astrophysics); Umetsu, Keiichi (Academia Sinica, Institute of Astronomy and Astrophysics); Stark, Dan (University of Arizona); Bradley, Larry (STSCI); Trenti, Michele (University of Melbourne); Johnson, Traci (University of Michigan); Bradač, Maruša (University of California-Davis); Dawson, Will (Lawrence Livermore National Laboratory); Rodney, Steve (University of South Carolina); Strolger, Lou (STSCI); Paterno-Mahler, Rachel (University of Michigan) Motivation Lensing Methods Future Work Preliminary Results Preliminary Results Acknowledgements Sample Selection Data • The epoch of reionization refers to the period ~1 billion years ago (z>6.5) when the neutral intergalactic medium was ionized by the first luminous sources • The Reionization Lensing Cluster Survey (RELICS) aims to discover >100 galaxies at z>9, crucial for understanding the epoch of reionization • Gravitational lensing by clusters of galaxies amplifies the light of background sources • We create lens models to quantify the magnification factor within these galaxy clusters • Obtain spectroscopic redshifts of arcs to better constrain lens model • Remodel each lens with spectroscopic redshifts • Generate magnification maps for each cluster to determine magnification in the FOV of the cluster • Repeat the process for all clusters • Lens models for each cluster are crucial for the interpretation of the measurements of background galaxies at high redshifts • Massive objects bend light, which causes gravitational lensing as seen in the figure below • Lensing magnifies background sources and makes it possible to find very distant objects • Strong lensing creates arcs, which are several magnified images of the same background source • We find these arcs and use them as constraints to model the cluster’s mass distribution • Lens models created for RXC0142+44, Abell2163 • Current lens models use photometric redshifts as constraints for the arcs • This can create systematic error in the magnification generated by each model by up to 20% • To reduce this error, spectroscopic redshifts need to be added • 3 or more spectroscopic redshifts can reduce this systematic error to <5% • Other sources for uncertainty include the number of multiply-imaged galaxies, substructure, and mass on the line of sight. • • 190 HST orbits will be used from 9/2015 to 4/2017 • 3 orbits for each cluster using ACS in F435W, F606W, F814W • 2 orbits for each cluster with WFC3/IR in F105W, F125W, F140W, F160W • Filters used range from 0.4-1.7 microns • 2 epochs for each cluster, separated by 25-60 days to enable variability search for SNe Support for program GO14096 was provided by NASA under contract NAS5-26555. A plot of galaxy clusters in the Planck SZ Mass catalog versus their redshift. Clusters observed by RELICS are marked in red. Most of the red boxes are concentrated in the high mass area. M 1600,AB log Number/mag/Mpc³ -2 -3 10 z~4 z~5 z~6 z~7 z~8 z~10 -4 -5 -6 -22 -20 -18 -16 Redshift Planck SZ Mass (10 Msun) 14 WFC3/IR NICMOS ACS/UVIS WFPC2 no HST Frontier Fields CLASH RELICS HST > 0.4 microns 0.0 0.2 0.4 0.6 0.8 1.0 18 16 14 12 10 8 6 4 2 0 A plot of the current luminosity function, which is well constrained out to z~8. The purple line, which indicates z~10, has much larger error bars than other redshifts becauase we lack data at these redshifts (Figure adapted from Bouwens et al, 2015) Lens model for RXC0142+44, constructed using four different sets of arcs as constraints. Overplotted in red are the critical curves for a source at redshift z=3.1, representing regions in the image plane with high magnification. Yellow curves are the projection of these lines in the source plane. Lens model for Abell2163, constructed using two different sets of arcs as constraints. Overplotted in red are the critical curves for a source at redshift z=2, representing regions in the image plane with high magnification. Yellow curves are the projection of these lines in the source plane. • We select 46 fields based on two criteria: 1) Most massive Planck clusters ( >4e14 Msun) 2) Evidence of exceptional strong-lensing effects • Seven clusters observed; lens models for three Expectation Arc 1.1 Arc 1.2 Arc 1.3 Arc 3.1 Arc 3.2 Arc 3.3 Redshift Redshift Redshift Redshift Uncertainties • A sample of the arc systems identified in RXC0142 and the plots of their photometric redshift probability distribution functions • When spectroscopic redshifts are not available, photometric redshifts are used as priors in the lens modeling process. References Bouwens et al (2015) ApJ, 803, 34 Johnson et al (2016), in prep Photometric redshift PDF from RELICS imaging data Credit: Dan Coe Figure credit: Traci Johnson Systematic error (not including statistical) # of spectroscopic redshifts Magnification error (magnitudes) 0 1 2 3 4 -0.3 -0.2 -0.1 0.0 0.1 0.2 0.3 0.4 0.5 0.6 Redshift Redshift Probability 3.5 3.0 2.5 2.0 1.5 1.0 0.5 0.0 0 1 2 3 0 1 2 3 0 1 2 3 0 1 2 3 4 0 1 2 3 0 1 2 3 8 7 6 5 4 3 2 1 0 7 6 5 4 3 2 1 0 7 6 5 4 3 2 1 0 Probability 10 8 6 4 2 0 10 8 6 4 2 0 Probability Probability Probability Probability 10% 5% 2% 20%
Transcript of Preliminary Lens Models for Massive Planck Clusters in the ...kerens/files/cerny_poster_2016.pdf ·...
Preliminary Lens Models for Massive Planck Clusters in the RELICS Survey Cerny, Catherine (University of Michigan); Sharon, Keren (University of Michigan); Coe, Dan (Space Telescope Science Institute [STSCI]); Jones, Christine
(Smithsonian Institution Astrophysical Observatory); Czakon, Nicole (Academia Sinica, Institute of Astronomy and Astrophysics); Umetsu, Keiichi (Academia Sinica, Institute of Astronomy and Astrophysics); Stark, Dan (University of Arizona); Bradley, Larry (STSCI); Trenti, Michele (University of Melbourne); Johnson,
Traci (University of Michigan); Bradač, Maruša (University of California-Davis); Dawson, Will (Lawrence Livermore National Laboratory); Rodney, Steve (University of South Carolina); Strolger, Lou (STSCI); Paterno-Mahler, Rachel (University of Michigan)
Motivation
Lensing Methods
Future Work
Preliminary Results
Preliminary Results
Acknowledgements
Sample Selection
Data • The epoch of reionization refers to the period ~1 billion years ago (z>6.5) when the neutral intergalactic medium was ionized by the first luminous sources• The Reionization Lensing Cluster Survey (RELICS) aims to discover >100 galaxies at z>9, crucial for understanding the epoch of reionization• Gravitational lensing by clusters of galaxies amplifies the light of background sources • We create lens models to quantify the magnification factor within these galaxy clusters
• Obtain spectroscopic redshifts of arcs to better constrain lens model• Remodel each lens with spectroscopic redshifts• Generate magnification maps for each cluster to determine magnification in the FOV of the cluster• Repeat the process for all clusters• Lens models for each cluster are crucial for the interpretation of the measurements of background galaxies at high redshifts
• Massive objects bend light, which causes gravitational lensing as seen in the figure below• Lensing magnifies background sources and makes it possible to find very distant objects• Strong lensing creates arcs, which are several magnified images of the same background source • We find these arcs and use them as constraints to model the cluster’s mass distribution
• Lens models created for RXC0142+44, Abell2163
• Current lens models use photometric redshifts as constraints for the arcs• This can create systematic error in the magnification generated by each model by up to 20%• To reduce this error, spectroscopic redshifts need to be added• 3 or more spectroscopic redshifts can reduce this systematic error to <5% • Other sources for uncertainty include the number of multiply-imaged galaxies, substructure, and mass on the line of sight.
•
• 190 HST orbits will be used from 9/2015 to 4/2017 • 3 orbits for each cluster using ACS in F435W, F606W, F814W• 2 orbits for each cluster with WFC3/IR in F105W, F125W, F140W, F160W• Filters used range from 0.4-1.7 microns• 2 epochs for each cluster, separated by 25-60 days to enable variability search for SNe
Support for program GO14096 was provided by NASA under contract NAS5-26555.
A plot of galaxy clusters in the Planck SZ Mass catalog versus their redshift. Clusters observed by RELICS are marked in red. Most of the red boxes are concentrated in the high mass area.
M1600,AB
log
N
umb
er/m
ag/M
pc³
-2
-3
10
z~4z~5z~6z~7z~8z~10
-4
-5
-6
-22 -20 -18 -16
Redshift
Pla
nck
SZ
Mas
s (1
0 M
sun)
14
WFC3/IRNICMOSACS/UVISWFPC2no HSTFrontier FieldsCLASHRELICS
HST > 0.4 microns
0.0 0.2 0.4 0.6 0.8 1.0
18
16
14
12
10
8
6
4
2
0
A plot of the current luminosity function, which is well constrained out to z~8. The purple line, which indicates z~10, has much larger error bars than other redshifts becauase we lack data at these redshifts (Figure adapted from Bouwens et al, 2015)
Lens model for RXC0142+44, constructed using four different sets of arcs as constraints. Overplotted in red are the critical curves for a source at redshift z=3.1, representing regions in the image plane with high magnification. Yellow curves are the projection of these lines in the source plane.
Lens model for Abell2163, constructed using two different sets of arcs as constraints. Overplotted in red are the critical curves for a source at redshift z=2, representing regions in the image plane with high magnification. Yellow curves are the projection of these lines in the source plane.
• We select 46 fields based on two criteria: 1) Most massive Planck clusters ( >4e14 Msun) 2) Evidence of exceptional strong-lensing effects• Seven clusters observed; lens models for three
Expectation
Arc 1.1 Arc 1.2 Arc 1.3
Arc 3.1 Arc 3.2 Arc 3.3
Redshift Redshift Redshift
RedshiftRedshiftRedshift
Uncertainties
• A sample of the arc systems identified in RXC0142 and the plots of their photometric redshift probability distribution functions• When spectroscopic redshifts are not available, photometric redshifts are used as priors in the lens modeling process.
ReferencesBouwens et al (2015) ApJ, 803, 34Johnson et al (2016), in prep
Photometric redshift PDF from RELICS imaging dataCredit: Dan Coe
Figure credit: Traci Johnson
5
Systematic error (not including statistical)
# of spectroscopic redshifts
Mag
nific
atio
n er
ror
(mag
nitu
des
)
0 1 2 3 4
-0.3
-0.2
-0.1
0.0
0.1
0.2
0.3
0.4
0.5
0.6
Redshift Redshift
Pro
bab
ility
3.5
3.0
2.5
2.0
1.5
1.0
0.5
0.00 1 2 3 0 1 2 3 0 1 2 3
0 1 2 3 4 0 1 2 3 0 1 2 3
8
7
6
5
4
3
2
1
0
7
6
5
4
3
2
1
0
7
6
5
4
3
2
1
0
Pro
bab
ility
10
8
6
4
2
0
10
8
6
4
2
0
Pro
bab
ility
Pro
bab
ility
Pro
bab
ility
Pro
bab
ility
10%
5%2%
20%
