Embed Size (px)
Citation preview
National Aeronautics and Space Administration!Cosmic Origins!Program Office"
!"#$!%&'()&%$*+,,-./%&$0$!-'/1$*2/%)2%$*+,,-./%&$3('/24$5-6-78$9:(6+;()$
!"#$%&'('")*+%%,('-'%."#'/'"%0#12'3%4#5')%C%,8*3'+%,#775%4'#9%
$<$
National Aeronautics and Space Administration!Cosmic Origins!Program Office"
!"#$!%&'()&%$*+,,-./%&$0$!-'/1$*2/%)2%$*+,,-./%&$3('/24$5-6-78$9:(6+;()$
!"#$%&'('")*+%%,('-'%."#'/'"%0#12'3%4#5')%C%,8*3'+%,#775%4'#9%
$=$
3
UV Time Domain Studies of Active Galactic Nuclei
STScI 18 September 2012
Bradley M. Peterson The Ohio State University
RJ Assef (JPL), MC Bentz (GSU), E Dalla Bontà (Padua), KD Denney (Dark), G De Rosa (OSU), S Frank (OSU), MR Goad (Leicester), CJ Grier (OSU),
K Horne (St Andrews), CS Kochanek (OSU), GA Kriss (STScI), A Marconi (Florence), S Mathur (OSU), A Pancoast (UCSB), M Pessah (NBI), RW Pogge (OSU), A Rafiee (Towson), T Treu (UCSB), M Vestergaard (Dark)
4
Reverberation Mapping
Grier et al. 2011, ApJ, 744, L4
Emission line variations follow those in continuum with a small time delay (14 days here) due to light-travel time across the broad-line region (BLR).
A Virialized BLR
•" !V " R –1/2 for every AGN in which it is testable.
•" Suggests that gravity is the principal dynamical force in the BLR. –" Caveat:
radiation pressure!
Peterson & Wandel 2002
Mrk 110
Kollatschny 2003
Bentz et al. 2009
5
6
Relationship Between BLR Radius and AGN Luminosity
Highest quality data only (as of 2009)
7
Reverberation-Based Masses
2BH /M f r V G= !
Observables: r = BLR radius (reverberation) !V = Emission-line width
Virial Product (units of mass)
Set by geometry and inclination (subsumes everything we don t know)
If we have independent measures of MBH, we can compute an ensemble average <f >
8
RM as a Cosmological Tool
Watson et al. 2011, ApJ, 744, L4
9
R-L for UV Lines (C IV #1549)
Few sources with C IV lags, and these are at least somewhat dubious
Kaspi et al. 2007, ApJ, 659, 997
10
Velocity-Delay Map Configuration
space Velocity-Delay
space
To observer Time delay
Doppler velocity
Broad-line region as a disk,
2–20 light days Black hole/accretion disk
Time after continuum outburst
Time delay
Line profile at current time delay
Isodelay surface
20 light days
11
12
13
Reverberation Response of an Emission Line to a Variable Continuum
The relationship between the continuum and emission can be taken to be:
Velocity-resolved emission-line
light curve
Velocity-delay map
Continuum light curve
Arp 151 LAMP: Bentz et al. 2010
Velocity-delay map is observed line response to a $-function outburst
( , ) ( , ) ( )L V t V C t d! ! != " #$
14
Optical Velocity Delay Maps Show Infall in Balmer Lines
Grier et al. 2012, in preparation
15
UV RM Programs 1)" Intensive monitoring to get UV velocity-delay
maps to establish flow of high-ionization gas •" Expect C IV to show outflow? •" Sampling (NGC 5548): once per day for 180 days •" For other sources, time sampling and duration both
scale as L1/2
2)" Moderately high cadence programs to establish C IV R-L •" Needed for high-z masses and cosmology
(z < 2 must be done from space) •" Sampling: ~40 observations, cadence and duration
as L1/2
•" Number of targets: ~7 (each 0.5 dex in range 41.0 % log #L#(1350Å) % 46.0)
16
Stellar and gas dynamics requires resolving the black hole radius of influence r*
Quiescent galaxies RM AGNs
National Aeronautics and Space Administration!Cosmic Origins!Program Office"
!"#$!%&'()&%$*+,,-./%&$0$!-'/1$*2/%)2%$*+,,-./%&$3('/24$5-6-78$9:(6+;()$
!"#$%&'('")*+%%,('-'%."#'/'"%0#12'3%4#5')%C%,8*3'+%,#775%4'#9%
$<>$
?2;:%$5-6-2;2$@+26%/$-)1$AB%/.$.(6%$/)$5-6-78$"(.,-;()$-)1$
9:(6+;()$$$$$
*A%:%$C.-%,%.$DEF?GH$!(I/%.$J/)1B(.&A$D?*FGH$C%))%AB$5K$E-.'%)A%.$D@?*?L5*"EGH$$$M/N%$E.%)&B-O$D5*FGH$M-.;)$96:/&$DEP?GH$-)1$M-.I-./A-$C-.(:&N-$DEP?G$$$$$$$$$$$$$$$Q.%&%)A%1$-A$AB%$FR#*$ES!$!"#$J(.N&B('$-A$*3*2#H$<T$*%'AKH$=U<=$
Q.%&%)A%1$-A$AB%$FR#*$ES!$!"#$J(.N&B('$-A$*3*2#H$<T$*%'AK$=U<=$
18
•" 3B%$?5@$'B-&%$/&$2./;2-6$/)$I-6-78$%:(6+;()$
•" $3B%$,-&&$(P$AB%$2%)A.-6$V6-2N$W(6%H$AB%$?5@$X%)I/)%Y$/&$2(..%6-A%1$O/AB$AB%$,-&&$(P$AB%$I-6-2;2$Z+6I%$
•" $*+II%&A&$AB-A$AB%$/I)/;()$(P$AB%$?5@$.%I+6-A%&$Z+/61L+'$(P$Z+6I%K$V+A$W(O[$
•" ?&$&B(O)$-A$./IBAH$AB%$?5@$2-)$-\%2A$AB%/.$&+..(+)1/)I&$(:%.$<=$(.1%.&$(P$,-I)/A+1%$/)$&/]%$D"/I+.%$P.(,$!K$V6-)1P(.1H$<^^UG$$
•" ?5@$P%%1Z-2N[$
•" $_0U`$(P$38'%$<$?5@$&B(O$%:/1%)2%$(P$,-&&$(+a6(O&$1%A%2A%1$:/-$FR$-)1$bL.-8$-Z&(.';()$D%KIK$E.%)&B-O$%A$-6K$<^^^c$C-&'/$%A$-6K$=UU<G$$
•" $!"#$%&'$()'*'$"+,-"#*$.&/0'1$%1.$#)'&'$."$()'2$%&/*'3$
$$
19
•" 3B%$?5@$2-)$/)d+%)2%$/A&$B(&A$I-6-78$-A$&2-6%&$.-)I/)I$A($M'2&K$W(O%:%.H$/)$(.1%.$A($P+668$'.(Z%$AB%$2./;2-6$.(6%$(P$AB%$?5@$/)$I-6-78$P(.,-;()e%:(6+;()H$1'#$4%5%6/-/7'*$%&'$&'8+/&'.$
•" Q.(Z/)I$AB%$/))%.$&A.+2A+.%$(P$?5@$.%f+/.%&$(';2-6eFR$/,-I/)I$-A$&+ZL,/66/-.2&%2()1$.%&(6+;()$•" E-)$()68$Z%$-2B/%:%1$O/AB$&'-2%LZ-&%1H$6()I$Z-&%6/)%$DUK0L<KU$N,G$(Z&%.:-A(./%&4$FReS';2-6$/)A%.P%.(,%A%.$DFRS#G$$$
@%O$3%2B)(6(I8$P(.$,+6;L%6%,%)A$$
$&'-.&%$-'%.A+.%$A%6%&2('%&$-)1$$
$/)A%.P%.(,%A%.&$P(.$FRS#4$
<K" Q.%2/&/()$P(.,-;()$d8/)I$(P$
$g$A($hU$&'-2%2.-i$
$=K$-+A()(,(+&$O-:%LP.()A$&%)&/)I$
$-)1$2()A.(6$(P$-..-8&K$
hK$M%AB(1(6(I/%&$P(.$I.(+)1LZ-&%1$
$:-6/1-;()$(P$6-.I%LZ-&%6/)%H$$
$,-)8$%6%,%)A$&8&A%,&K$20
*2/%)2%$!%f+/.%,%)A&$•" FReS';2-6$*'%2A.-6$#,-I/)I4$AB%$&2/%)2%$I(-6$/&$A($,-'$AB%$%,/&&/()L6/)%$
&A.+2A+.%$(P$AB%$(+A%.$V.(-1$j/)%$!%I/()$:/-$)-..(OLZ-)1$/,-I/)I$(P$FR$6/)%&H$%KIK$j8LkH$E#R$<00UlH$MI$##$=TUUlK$E();)++,$/,-I%&$-.%$.%f+/.%1$-A$)%-.Z8$O-:%6%)IAB&$P(.$2();)++,L&+ZA.-2;()K$!%L(Z&%.:-;()&$()$,()AB68$;,%&2-6%&$O/66$Z%$&+m2/%)A$P(.$'.(Z/)I$2B-)I%&$/)$AB%$%,/&&/()L6/)%$I-&K$
•" "/%61$(P$R/%O4$n$o$b$o$,-&$•" -)I+6-.$.%&(6+;()4$_UK<$,-&$
•" !%f+/.%&$(+A%.$'./,-.8$,/..(.$1/-,%A%.&$(P$-A$6%-&A$_$0UU,$•" *'%2A.-6$.%&(6+;()4$_<Ul$
•" E(..%&'()1&$A($=UUU$N,e&%2$P(.$E#R$<00UlK$V%p%.$.%&(6+;()$O(+61$Z%$1%&/.-Z6%$
•" J-:%6%)IAB$Z-)1D&G$•" <=UULhUUUl$P(.$2();)++,$/,-I%&$$$•" @%%1$)-..(O$Z-)1&$_<Ul$-.(+)1$%,/&&/()$6/)%&K$•" M%1/+,$Z-)1&H$_<UUlH$P(.$2();)++,$&+ZA.-2;()$
•" *%)&/;:/A8$•" ?Z/6/A8$A($1%A%2A$0KU7<UL<o$%.I&e2,=e&%2$/)$E#R$<00Ul$
$
21
National Aeronautics and Space Administration!Cosmic Origins!Program Office"
!"#$!%&'()&%$*+,,-./%&$0$!-'/1$*2/%)2%$*+,,-./%&$3('/24$5-6-78$9:(6+;()$
!"#$%&'('")*+%%,('-'%."#'/'"%0#12'3%4#5')%C%,8*3'+%,#775%4'#9%
$==$
97A.-I-6-2;2$j8,-)L-6'B-$97'%./,%)A&$/)$AB%$@%-.Z8$F)/:%.&%$
M-pB%O$Wk8%&$$
O/AB4$5(.-)$S&A6/)H$qLM/I+%6$M-&LW%&&%H$W%2A(.$S;L"6(.-)%&H$r-)/%6$C+)ABH$r-)/%6$
*2B-%.%.H$?))%$R%.B-,,%$
=h$
*2/%)2%$E()A%7A$
•" j8-$,-s(.$&'%2A.(&2('/2$'.(Z%$t$B/IBL]$•" ?6,(&A$=$1%2-1%&$(P$O(.N$1()%$-A$]n=$$•" Q.(Z%&$D(.$2(+61$'(A%);-668G4$$
–"j(O%&A$,-&&$I-6-7/%&$-A$-)8$%'(2B$–"E(&,/2$O%Z$–"r-.N$26(+1&$–"Q('+6-;()$###$
•" !%:%-6&$,+2B$-Z(+A$%:(6+;()$(P$I-6-7/%&H$1+&A$2()A%)A&H$%:(6+;()H$.%/()/]-;()$%A2$$
=o$
*2/%)2%$E()A%7A$#$u$=eh$(P$2(&,/2$;,%$
0.2 0.3 0.5 0.7 1 2 3 5 7redshift
10−3
10−2
10−1
100
f esc
(Lyα
)
Co 10Ha 10Ca 10Gr 07Ou 08Da 07Sh 09Iy 06Ou 10Hi 10
MH+2011
Barger+2012
Bouwens+201*
=0$
*2/%)2%$E()A%7A$#$u$=eh$(P$2(&,/2$;,%$
0.2 0.3 0.5 0.7 1 2 3 5 7redshift
10−3
10−2
10−1
100
f esc
(Lyα
)
Co 10Ha 10Ca 10Gr 07Ou 08Da 07Sh 09Iy 06Ou 10Hi 10
MH+2011
Bouwens+201*
Barger+2012
=g$
E+..%)A$&B(.A2(,/)I&$#$
•" j-p%.$=eh$D]v=G$(P$2(&,/2$B/&A(.8$)(A$2(:%.%1$D/)26+1%&$-66$AB%$1%26/)%$(P$*"!rG$$
•" E-))(A$1%A%.,/)%$j8-$j"$w$9J$1/&A./Z+;()$#(%#+5%"'$)2:;$OB%.%$O%$2-)$-6&($1%A%.,/)%$OB-A$'.(2%&&%&$&B-'%$AB%,x$
•" j8-$.%&()-)2%$6/)%$u$32#(%$:8(#(')%("#+)9*"(<%%
1"$('-'*4"5'$4%1$."$%$.''5$6-/1.$9:$*+&0'2$=>$
*+.:%8/)I$j8-$A($]$y$=$•" "/66$/)$j8-$&A-;&;2&$-A$]$_$UKh$z$=$$
–"9:$*+&0'2$('-'*4"5'$•" Q.(Z-Z68$&'%2A.('B(A(,%A.8$e$&6/A6%&&$&'%2A.(&2('8$•" r%A%2A$_<Uh$I-6-7/%&$Z8$j8-$&%6%2;()H$-)1$_<Uo$Z8$FR$!$&%:%.-6$Z/)&$(P$&%:%.-6$B+)1.%1$I-6-7/%&$$•" Q.(Z%$A($v$<U`$j{$-A$-)8$I/:%)$.%1&B/i$Z/)$
–";+</-/%&2$.%(%$•" S';2-6e@#!$&'%2A.-$u$"/Z%.$&'%2A.(I.-'B&$e$9FEj#r$•" r%%'$&+.:%8$/,-I/)I$$|%61&$u$W*3$}$$•" r/.%2A$W#$,%-&+.%,%)A&$}$[$
=T$
*+.:%8/)I$j8-$A($]$y$=$•" r%A-/6%1$FR$(Z&%.:-;()&$(:%.$&-,%$.-)I%$
–"='*"-0'.$*5'4(&"*4"52$%&"+1.$>2%$•" FR$-Z&(.';()$6/)%&$!$I-&$2(:%./)I$P.-2;()&H$&A%66-.$'('+6-;()&H$N/)%,-;2&$•" W/IB%.$=%1/&'%.&%.H$|%61$.%&A./2;()&$~,(:%-Z6%$&6/A&H$,/2.(&B+p%.$-..-8H}�$[$$
–"!/?)@&'*"-+7"1$A1%&&"#6%1.$/B%?/1?C$•" '.(Z%$:%.8$P-/)A$B-6(%&H$.%2(:%.$I6(Z-6$d+7%&H$A%&A$%m2/%)28$(P$&2-Ä)I$•" *,-66L&2-6%$:-./-;()&$/)$&A.+2A+.%$(P$#*M$•" W-6($.%1&B/i$%:(6+;()$$
=^$
3%2B)/2-6$!%f+/.%,%)A&$$•" M(&A68$*'%2A.(&2('8H$Z+A$&(,%$/,-I/)I$2-'-Z/6/;%&$4$$
–" &6/A6%&&$&'%2A.('B(A(,%A.8$u$%m2/%)A$&+.:%8/)I$P.(,$.%1&B/i$2(:%.-I%$–" #)A%.,%1/-A%$=$&'%2A.(&2('8$u$1%A-/6%1$'B8&/2-6$'.('%.;%&$~&6/A&$(.$&/,/6-.�$
•" "/%61D&G$(P$R/%O$4$$–" "/1+2/-6$&+.:%8$4$)%%1$n_UK<$1%I=K$*+.:%8$2-,%.-$"(R$n_$hU$-.2,/)=$–" W/IB%.$.%&(6+;()$,(1%&$2-)$(P$2(+.&%$,%$&,-66%.$
•" QB8&/2-6$e$-)I+6-.$.%&(6+;()D&G$–" r/\.-2;()L6/,/A%1$'%.P(.,-)2%$)(A$)%2%&&-.8K$_UKU0$-.2&%2$$
•" *'%2A.-6$.%&(6+;()D&G$–" !$_$<UU$&'%2A.(&2('8$P(.$&+.:%8/)I$–" !$_$0HUUU$&'%2A.(&2('8$P(.$1%A-/6%1$&A+1/%&$
•" J-:%6%)IAB$Z-)1D&G$–" <0UU$z$hgUU$??H$'.%P%.-Z68$1(O)$A($.%&a.-,%$j8L-6'B-$
•" *%)&/;:/A8$–" #)A%I.-A%1$6/)%$d+7$1(O)$A($_%L<g$2I&$P(.$&+.:%8$$
hU$
National Aeronautics and Space Administration!Cosmic Origins!Program Office"
!"#$!%&'()&%$*+,,-./%&$0$!-'/1$*2/%)2%$*+,,-./%&$3('/24$5-6-78$9:(6+;()$
!"#$%&'('")*+%%,('-'%."#'/'"%0#12'3%4#5')%C%,8*3'+%,#775%4'#9%
$h<$
Paul Scowen (ASU) Rolf Jansen, Rogier Windhorst, James Rhoads, Sangeeta Malhotra, Daniel
Stern, Robert O’Connell, Matt Beasley
GALAXY ASSEMBLY AND SMBH/AGN-GROWTH
32
MOTIVATION •" To address the question: How did galaxies evolve from the very first systems to the types
we observe nearby?
•" Driven by the recent advances in understanding the high redshift Universe, with many objects being found at z>6 and the need to understand Reionization
•" The co-called “Cosmic Dawn” era represents the period (z=6-8) when the hydrogen reionization was complete
•" During this period the first stars and galaxies formed, but there is a fundamental lack of understanding about how this happened – the lack of original metals means that cooling processes were very different
•" Objects at z>7 are very faint and very rare – need widefield imaging and diffraction limited optics to be able to find and characterize targets
33
SPECIFIC COMPONENTS •" Evolution of the faint-end slope of the dwarf galaxy (DG) luminosity function (LF):
•" Due to steepening of the LF slope, it is possible that reionization could have been achieved by DG-generated ionizing photons – the critical quantity to understand is the escape fraction – the survey would answer this question with a statistically significant sample
•" Tracing the Reionization history using Ly-! emitters: •" A medium band survey would derive the LF of Ly-! emitters at z>5.5 over a wide
angular area for a large sample – and address the evolution of the reionization of the IGM over time
•" Lyman-continuum escape fraction of DGs and weak AGN: •" We expect the escape fraction to be higher at higher redshifts because of the lack of
metals – however this places a limit on how soon DGs could have started shining without removing all neutral-H in front of z=6 QSOs. This implies a downturn in the LF at z>6.5, which represents a rapid onset of the cosmic SFR between z=6-8
34
SPECIFIC COMPONENTS •" Hierarchical Galaxy Assembly:
•" Despite advances provided by the HST deep fields, the fine details of how galaxies assembled over z=0.5-5 are not understood
•" Better spatial sampling, depth and larger fields of view are needed – our survey would provide robust spectrophotometric redshifts for more than 5 million galaxies with mAB ~28-30 mag with resolution down to a few kpc
•" Epoch-dependent merger rates of galaxies: •" Using the sample from above, we can trace the pair fraction and galaxy major merger rate
down to mAB > 27 •" Our survey would allow the mapping of the entire epoch-dependent merger rate history a
full 3 mags fainter than has been possible •" Growth of super-massive black holes (SMBHs):
•" Using variability, our survey could measure the weak AGN fraction in more than 105 galaxies, down to mAB ~28-30 mag at z<8 and thereby constrain how SMBH growth kept pace with galaxy assembly
35
FOUR CENTRAL QUESTIONS •" How did reionization progress during the era of ‘Cosmic Dawn’? Was it an extended, a
rather abrupt, or even a multiple event?
•" How did the faint end of the galaxy luminosity function evolve from the onset of Pop II star formation till the end of the reionization epoch?
•" How exactly did AGN and SMBH growth keep pace with the process of galaxy assembly?How did AGN growth decline with the galaxy merger rate and the cosmic SFR?
•" Was there indeed an epoch of maximum merging and AGN activity around z 1–2 for the more massive galaxies, before the effects from the increasingly dominant Dark Energy kicked in? How does this peak epoch depend on galaxy total mass or bulge mass, and (how) does this support the galaxy downsizing picture?
36
National Aeronautics and Space Administration!Cosmic Origins!Program Office"
!"#$!%&'()&%$*+,,-./%&$0$!-'/1$*2/%)2%$*+,,-./%&$3('/24$5-6-78$9:(6+;()$
!"#$%&'('")*+%%,('-'%."#'/'"%0#12'3%4#5')%C%,8*3'+%,#775%4'#9%
$h>$
;$9:DE574%-DF'%&@G=$H5'4(&"*4"5/4$HI2$H+&0'2$J"&$91.'&*(%1./1?$K%-%<2$L0"-+7"1$
$
*-668$W%-'H$q%\.%8$C.+NH$q-)%$!/IZ8$D@?*?’&$5*"EGH$M-&&/,($!(Z%.A($D*3*2#G$
H"+&4'*$5+))wU^H$“F)1%.&A-)1/)I$AB%$-&A.('B8&/2&$(P$I-6-78$%:(6+;()4$AB%$.(6%$(P$$$$*'%2A.(&2('/2$&+.:%8&$/)$AB%$)%7A$1%2-1%”H$OB/A%$'-'%.$&+Z,/p%1$A($?&A.(=U<U$966/&w<=H$“97A.-I-6-2;2$&2/%)2%$-)1$2(&,(6(I8$O/AB$AB%$*+Z-.+$Q"*”H$$$$-&A.(L'Be<=UgKU>h>:=$
hT$
*2/%);|2$5(-6$Å$#):%&;I-;()$
,8:'+>?8%@*#7)4$3($+)1%.&A-)1$B(O$I-6-7/%&$%:(6:%1$A($P(.,$AB%$P-,/6/-.$W+ZZ6%$&%f+%)2%$(P$&'/.-6&$-)1$%66/';2-6&$-)1$A($%&A-Z6/&B$OB/2B$'.(2%&&%&$O%.%$.%&'()&/Z6%K$$,8:'+>?8%A+-')>B#>*+4$3($2()1+2A$-$UK=L<K>µ &'%2A.(&2('/2$&+.:%8$(P$-A$6%-&A$<Ug$I-6-7/%&$-A$]nUKT$/)$-$,/&&/()$6-&;)I$h$8%-.&$$C25%,9'8("#<%S)68$&'%2A.-$2-)$'.(:/1%4$•"$-22+.-A%$.%1&B/i&$P(.$2(-11/;()H$/1%);|2-;()$(P$26+&A%./)I$•"$26%-)$&%'-.-;()$(P$2();)++,$Å$%,/&&/()L6/)%$d+7$•"$N/)%,-;2&$(P$I-6-7/%&$-)1$I-6-78$26+&A%.$18)-,/2&$•"$1+&A$'.('%.;%&$D%7;)2;()$2+.:%G$$•"$'B8&/2-6$2()1/;()&$(P$AB%$#*MH$E5M$-)1$#5M$•"$%:(6+;()$(P$AB%$,-&&L,%A-66/2/A8$.%6-;()$•"$2(L%:(6+;()$(P$I-6-7/%&$Å$Z6-2N$B(6%&$$C25%,*%0#+5%@#7#D:')<%3($1/&;)I+/&B$-,()I$AB%$%\%2A&$(P$-22.%;()H$,%.I%.&H$&A-.$P(.,-;()$-)1$P%%1Z-2NH$I.(OAB$(P$Z6-2N$B(6%&c$-)1$A($2(:%.$-$O/1%$:-./%A8$(P$%):/.(),%)A&$AB-A$I(:%.)$&A-.$P(.,-;()K$
h^$
JB8$“()68”$_<$,/66/()$I-6-78$&'%2A.-[$$
j%&&()&$P.(,$*r**4$$D<G$#1%);P8$AB%$&2/%);|2$.%f+/.%,%)A&$)%%1%1$A($-)&O%.$AB%$&2/%);|2$f+%&;()$D=G$#1%);P8$AB%$/)&A.+,%)A-;()$)%%1%1$A($,%%A$AB%$&2/%);|2$.%f+/.%,%)A&$ oU$
S+.$'.('(&%1$&+.:%8$/&$:%.8$-,Z/;(+&4$ $ $A($P(66(O$()$P.(,$*r**$
Bp'4ee&1&&=UUTK+2B/2-I(K%1+e1%'(AeI+))Ls-,%&K'1P$o<$
3B%$'.('(&%1$FRL@#!$&'%2A.(&2('/2$&+.:%8$O/66$Z%$,(.%$'(O%.P+6$AB-)$*+Z-.+eQ"*$
=UUU$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$=UUUU$
$$$$$$
$
*+Z-.+eQ"*$
JB8[$V%2-+&%$(P$O/1%.$&'%2A.-6$.-)I%$DFRL@#!G$-)1$)($-A,(&'B%./2$'.(Z6%,&$ o=$
3B%$FRL@#!$*'%2A.(I.-'B$W-&$o$EB-))%6&$$
$$
$$$
$$
$$
=UUU$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$=UUUU$
$$$FR$$$$$$$$$$$$VjF9$$$$$$$$$$$$$!9r$$$$$$$$$$$$@#!$!_oUU$$$$$$$$!_oUU$$$$$$$$$$$!_oUU$$$$$$$$$!yoUU$!.%&A_<Uh$$$$$!.%&A_<Uh$$$$$$$$$$!.%&A_<Uh$$$$$$$$$$!.%&A_<Uh$$$$
$oh$
*2/%);|2$R-6+%$(P$FRL@#!$*'%2A.+,$
$$
$$$
$$
$$
=UUU$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$=UUUU$
@(A$s+&A$.%1&B/i&H$OB/2B$-.%$%-&8$A($,%-&+.%$P.(,$%,/&&/()$6/)%&H$Z+A$f+-);A-;:%$/)P(.,-;()$()$%-2B$I-6-78’&$&A-.&H$I-&H$1+&A$w$E5M$w$#5M$
oo$
$#)&A.+,%)AeQ%.P(.,-)2%$!%f+/.%,%)A&$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$
$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$=%1?'$+1.'&$*(+.2$•" 3%6%&2('%$r/-,%A%. $ $ $ $UK0L=Ko$,$•" SZ&%.:-;()$A8'% $ $ $ $ $MS*$*'%2A.(&2('8$w$#,-I/)I$$•" "/%61D&G$(P$R/%O $ $ $ $ $&yUK<0$u$UKUh$&fK$1%I$ $$•" ?)I+6-.$.%&(6+;()$ $ $ $ $UK^o”$u$UKh^”$$$$$DrMr$,/..(.$&/]%G$•" *'%2A.-6$.%&(6:/)I$'(O%. $ $ $oUUL<UUU$ $ $$•" J-:%6%)IAB$Z-)1&$ $ $ $o$2B-))%6&$A(I%AB%.$2(:%./)I$UK=L<K>µ'•" *%)&/;:/A8 $ $ $ $ $ $*e@$'%.$!9y>$/)$2();)++,$•" r8)-,/2$.-)I%$ $ $ $ $ $EErH$ME3$1%A%2A(.&$•" SAB%.$.%f+/.%,%)AD&G $ $ $ $n=0Ub$&+''.%&&/()$(P$](1/$(:%.$&6/A6%&&
$ $ $ $ $$$$$$$$$$$$ $ $ $M+6;L(Zs%2A$&6/A$&%6%2A(.$DrMr[G$$ $ $ $ $ $ $ $$$$$$$$ÇoUU$I-6-78$&'%2A.-$'%.$%7'(&+.% $$
$
o0$
@%7A$*A%'&4$*2/%);|2$Å$3%2B)(6(I8$*A+1/%&$HMGLFNGJGM$HN9OGLH$$É"%C2#(%:)%(2'%)/#77')(%('7')8*9'%AB-A$2-)$I%A$I((1$&'%2A.-$D*e@y>$'%.$!9G$(P$-A$6%-&A$<$,/66/()$]yUKTL=KU$I-6-7/%&[$$M-N%$&/,+6-;()&$+&/)I$AB%$E(&,(&$M(2N$E-A-6(I$A($|)1$(+AK$${$E#+%#%FGHIA=%)9'8("*)8*9:8%)6"-'5%2'79%(*%)*7-'%*(2'"%9"*J7'/)[#):%&;I-A%$(AB%.$-''6/2-;()&H$%KIK$%7;)2;()$2+.:%&$D5(.1()wGH$j8E$%&2-'% $$$P.-2;()$DM2E-)16%&&wGH$j8-$DM-.;)wGH$,-&&/:%$&A-.&$DJ(\(.1wG$ $ $ $$$/)$]y<L=$I-6-7/%&$$NLM!FE>EKP$HN9OGLH$${$A)%#%K0KHJ#)'$%)9'8("*)8*9:8%)6"-'5%L'#):J7'<%*A.-O,-)$&6/A$&%6%2A(.$/&$-$=UUU7<UUU$,/2.(,/..(.$-..-8$$
$DrMrG$('%.-;)I$-A$LoU$(E$DP(.$1-.N$&+''.%&&/()G$O/AB$$$-$O/)1(O$DP+&%1$&/6/2-[G$AB-A$A.-)&,/A&$6/IBA$(:%.$
$$$$$$$$UK=L<K>µ$r%:%6('$-)1$/,'6%,%)A$-$'6-)$A($Z./)I$AB%$rMr$A($3!j$g$$$
og$
V-2N+'$*6/1%4$J"#!*3$*'%2A.(&2('8$Å $ $ $FRL@#!$*'%2A.(&2('/2$*+.:%8$
9:@FG=$H5'4Q$H+&0'2$ RJG=HN$
*2/%);|2$5(-6$ S';,/]%1$P(.$<$I(-6$ M+6;'6%$I(-6&$
3%6%&2('%$$ <L,$26-&&$ <Kh$,$
S.Z/A$ *+)L&8)2K$(.Z/A$-A$>UU$N,$ *+)L9-.AB$j=$
Q./,-.8$,/&&/()$ h$8%-.&$ 0$8%-.&$
*'%2A.(I.-'B&$ o$MS*$*-/($&'%2A.(I.-'B&$ *-/(-'**$&'%2A.(&2('8$
J-:%6%)IAB$2(:%.-I%$ UK=L<K>$µ' UK>L=Ko$µ[$
SZ&%.:-;()$ r%%'$%7'(&+.%$Dnh$B.G$A($,%-&+.%$&A%66-.$2();)++,$
M%1/+,$%7'(&+.%$A($,%-&+.%$%,/&&/()L6/)%$#'
j/,/;)I$P-2A(.$ Q.(Z-Z68$1-.N$)(/&%$ W/IB$](1/$Z-2NI.(+)1$
J"#!*3$-)1$FRL@#!$*'%2A.(&2('/2$*+.:%8$-.%$2(,'6%,%)A-.8$o>$
National Aeronautics and Space Administration!Cosmic Origins!Program Office"
!"#$!%&'()&%$*+,,-./%&$0$!-'/1$*2/%)2%$*+,,-./%&$3('/24$5-6-78$9:(6+;()$
M9'+%K:)86)):*+$
oT$
