2016
Publication Year
2020-05-25T14:14:26Z
Acceptance in OA@INAF
AGN populations in GOODS-N through eMERGE ultra-deep JVLA observations
Title
GUIDETTI, DARIA; BONDI, MARCO; PRANDONI, ISABELLA; Beswick, R. J.; Muxlow, T. W. B.; et al. Authors 10.5281/zenodo.60452 DOI http://hdl.handle.net/20.500.12386/25148 Handle
and M . B ondi , I .P ra ndoni (IRA -IN A F, B ol ogna ) R .J . Be sw ic k, T.W .B . M uxl ow , N . W rigl ey (J odr ell B ank O bs er va tor y, U ni v. of M anc he ste r), I.R . Sm ail (Ins tit ut e for C om put ati ona lC os m ol ogy , D ur ha m U ni v.) , I. M cH ar dy (S chool of P hys ic s and A str onom y, U ni ve rs ity of S out ha m pt on) , R . I vi son (Ins tit ut e for A str onom y, U ni v. of E di nbur gh , R oya lO bs er va tor y) A nd t he eM E R G E col la bor ati on
Da
ria
G
ui
de
tti
Ist
itut
o di
R
adi
oa
str
onom
ia
-IN
A
F, B
ol
ogna
G a rc hi ng , J un e 3 0 , 2016AG
N
popul
at
ions
in
G
O
O
DS
-N
th
ro
ug
h
eM
E
R
G
E
ul
tra
-deep
JV
LA
o
bse
rva
tio
ns
A
c
om
pl
ete
c
ens
us
of
fa
int
AGNs
in
di
sta
nt
ga
la
xi
es
is
cruc
ia
lto
unde
rs
ta
nd
AGN
fe
edba
ck,
ac
cre
tion
re
gi
m
e a
nd
pos
sibl
e
co
-e
vol
ut
ion
w
ith
SF
pr
oc
es
se
s
R
adi
o
sur
ve
ys
inc
re
as
ingl
y
im
por
ta
nt
à
unbi
as
ed
and
re
sol
ve
d
vi
ew
of
AGNs
&
SF
C
om
pos
ite
sub
-mJ
y
ra
di
o
sour
ce
popul
ati
on
RQ
AGNs
sta
rt t
o
appe
ar
at
µJy
le
ve
ls
in
de
ep
ra
di
o
Fie
lds
(e .g. S eym our + 08, P adova ni + 09, + 11, + 15 B onz ini + 13 )8
kpc
1. 4 G H z M E R L IN on H S T AC S i ba nd Sta r f or m ati on 5. 5 G H z 0. 2 arcs ec -> ra di o A G N c or e ( G ui de tti + 15) Z~ 2 Ul tra -de ep ra di o obs . (~ µ Jy rm s) w ith hi gh spa tia l re sol ut ion (s ub -kpc → kpc ) all ow us to study the ove ra ll AGN popul ati on and di sti ngui sh ext ende d kpc sc ale S F e m iss ion from m or e c om pa ct A G N com pone nt s (< 1 kpc )C
ont
ext
Pa dova ni +15A
ve
ry
de
ep di
re
cte
d
sur
ve
y of
the
µJ
y
ra
di
o s
our
ce
popul
ati
on
in
GOODS
-N
m
or
phol
ogi
ca
lly
and
spe
ctr
all
y
ide
nt
ifi
ca
tion
of
A
G
N
s &
S
Fgs
up
to z
~5
400
hr
s
eM
ER
LI
N
+
J
V
L
A
@
1.4 G
H
z
378
hr
s
eM
ER
LI
N
+
JV
L
A
@
5 G
H
z
(P
I
Pr
andoni
)
re
sol
ut
ion
50
-2000 m
as
(
0.5
-te
ns
of
kpc
at
z
>
1)
w
ith 0.5
-1
µJ
y/b
rm
s
anc
ill
ar
y
cove
ra
ge
of
G
O
O
D
S-N
fr
om
ra
di
o
to X
-ra
y
5
G
H
z J
V
L
A
A
/B
sur
ve
y
[c
om
pl
ete
]
(G
ui
de
tti+
I
&
II
in
pr
ep)
1.
4
G
H
z J
V
L
A
-A
(39
hr
s)
[c
om
pl
ete
]
(O
w
en+
in
pr
ep)
1.
4
G
H
z (
20
da
ys
, 15%
da
ta
re
duc
ed)
&
5
G
H
z eM
E
R
L
IN
(Q2
->
2016)
T
he
eM
E
R
G
E
sur
ve
y
eM
E
R
LI
N
G
al
ax
y
E
vol
ut
ion
sur
ve
y
5 P
I P
R
A
N
D
O
N
I
St
at
us
G
oal
H
ow
P I M uxl ow , S m ail & M cH ar dy a nd 60 C O -is fr om 9 count rie s5.5 G
H
Z
JV
L
A
MO
S
A
IC
7-poi
nt
ing
m
os
aic
in
GOODS
-N
(m
atc
hi
ng
the
5
G
H
z e
-ME
R
L
IN
F
oV
)
14+
2
hour
s i
n
A
rra
y
A
&
B
[P
I:
M
uxl
ow
]
(Oc
t2012
&
Oc
t. 2013)
C
ent
ra
l f
re
que
nc
y
5.
5
G
H
z ,
2
G
H
z
ba
ndw
idt
h
0.5
ar
cs
ec
re
sol
ut
ion
, ~
1
µJ
y
rm
s
at
ce
nt
er
(1 s
igm
a)
50 % a re a rm s < 3 µJ y94 sour ce s (S /N >5) , at <7 ar cm in from the ce nt re
S
5. 5G H z > 6 µJ y, 50% w ithS
5. 5G H z< 30 µJ y 88% (83/ 94 ) s ec ur e Ks inde nt ifi ca tions w ithi n <0.5 ” (WI R C am , 5 σ de pt h of Ks ,A B = 24.45, W ang+ 10) 95% (79/ 83) w ith re ds hi ft (51 spe c 28 phot ) (C ow ie + 01,W irth+ 04,B arge r+ 08, K aji sa w a+ 10 , M om che va + 15) Fi rs t c ont our @ 3 σ 10 kpc 20 kpc 10 kpc5.5 G
H
z c
ata
logue
<si ze > ~ 0.4 ar cs ec (~ 3 kpc at z =1 )z
me d ~1 All P hot5
IR
c
ol
our
-c
ol
our
pl
ot
s (
N
IR
->
F
IR
)
qua sa r m ode AGNs , pa ss ive (r adi o m ode ), sta r f or m ing ga la xi esL
x-ra yqua
sa
r m
ode
AGNs
ra
di
o
exc
es
s
sour
ce
s
(D el M or o+ 13)ra
di
o
A
G
N
(R
M
&
Q
M
)
VL
B
I de
te
cti
ons
ra
di
o
A
G
N
(R
M
&
Q
M
)
M
ul
ti-!
cla
ss
ifi
ca
tion
of
the
5.5 G
H
z s
our
ce
s
S
am
pl
es
of
qua
sa
r/r
adi
o
m
ode
AGNs
and s
ta
r f
or
m
ing
ga
la
xi
es
IR
c
la
ss
ifi
ca
tion
of
the
5.5 G
H
z s
our
ce
s
■
35
AGNs
(qua
sa
r m
ode
) 45%
▲
15 pa
ss
ive
ga
la
xi
es
20%
●
27
SF/
hyb
sys
te
m
s
35%
5 I R CC cr iter ia St er n+ 05 (IR A C ), D onl ey+ 12 (IR A C ) K irkpa tri ck+ 12 (IR A C , 24 µm , 100µ m , 250µ m ) M es sia s+ 12 (Ks -ba nd, IR A C ) 3 a cc ount for re ds hi ft evol ut ion 94% (77/ 83) IR -cl as sif ied sour ce s 93% (77/ 83) of the Ks -ide nt ifi ed sour ce s w ith 4-IR A C ba nds da ta (W ang+ 10) 78% (65/ 83) M IR , F IR H er sc he l+ PE P da ta (E lba z+ 11, M agne lli + 13) Do nle y+ 12 La cy +0 7■ 44 Q M AGNs 57% ▲ 15 RM AGNs 20% ● 18 SF/ hyb 23% X -ray for 63% (52/ 83) (X ue + 16 ), 100 µ m for 63% (52/ 83) (E lba z+ 11, M agne lli + 13) , 1. 4 G H z V L A for 100% (M or ris on+ 10) , 1. 6 G H z VLB I (C hi + 13, R adc lif e+ 15)
X
-ra
y
&
ra
di
o
AGNs
■
35 Q M AGNs ▲ 15 R M AGNs ● 27 SF/ hyb QM AGNs if : Lx [2 -7 ke V ] > 10 42 er g/ s Lx [0. 2-7 ke V ] > 3× 10 42 er g/ s (for upp limits ) 29 X -ra y QM AGN (30% not IR Q M AGNs ) ra di o exc es s sour ce s if : q100 (log [S 100µ m /S 1. 4G H z ]) < 1.5 (D el M or o+ 13) S 100µ m= 1m Jy (3 sigm a) for uppe r limits 31 r adi o exc es s ( ~ 10% not IR R M A G N ) 1.6 GHz VL B I 18 sour ce s (~ 10% not IR R M AGNs )77%
of
t
he
c
las
sif
ie
d
sou
rc
es
ar
e AG
Ns
!!
× X-ra y AG N s~ 78% of the sour ce shos ta n A G N ( R M +Q M ) AGNs ove r al lz & L 5. 5G H z at z> 1.5 > 90% (34/ 37 sour ce s) are AGNs 3 S F/ hyb at z> 1.5 a re s ub -mm ga la xi es (B ar ge r+ 12) AGNs dom ina te dow n to fe w µ Jy (m os tQM ) ■ 44 Q M AGNs ▲ 15 RM AGNs ● 18 SF/ hyb AG N s SF /h yb al l
AGN
cont
ent
in t
he
5.5 G
O
O
D
S
-N
ca
ta
logue
1.4
-5.5 G
H
z s
pe
ctr
al
inde
x
&
opt
ic
al
im
age
s
z~ 1. 3 z~ 0. 5 10 kpc p as sive p as sive AGN AGN SF /h yb SF /h yb z~ 0.9 10 kpc z~ 0.5 z~ 1.5 z~ 1 z~ 0.6 1.4 G H z i nf or m ati on from V L A ca ta logue (1.7” F W H M M or ris on et al. 2010 ) Spe ctr al ana lys is limite d to com pa ct sour ce s: 61 w ith si ze <1 ar cs ec (~ 8 kpc @ z=1 ) 5. 5 G H z c ont our s/ H S T I ba nd im age z~ 0.5 10 kpc 10 kpc 10 kpc 10 kpc■
31 QM AGNs α me d ~ 0.73 ▲ 14 R M A G N ~ 0.40 ● 16 SF/ hyb sys te m s ~ 0.72S
" " -#■
142 Q M AGNs ▲ 34 RM AGNs ● 86 SF/ hyb sys te m s ~35%■
44 Q M AGNs ▲ 15 RM A G N ● 18 SF/ hyb sys te m s ~20%1.4 G
H
z se
le
cte
d
sa
m
pl
e
5. 5G H z s el ec ted sou rc es 1. 4 G H z s el ec ted sou rc es]
~65 %]
~80 % a la rge rf ra cti on of S F/ H yb and st ee p spe ctr a (84% ßà 49% at 5.5 G H z ) but AGNs st ill dom ina te from V L A c ata logue (1.7” F W H M M or ris on+ 10) 300 1.4 G H z s our ce s se le cte d in t he sa m e ar ea of our 5.5G H z m os aic (99% 20 µ Jy> S 1. 4G H z >1m Jy )Sum
m
ary
Fi rs t c ata logue of r adi o sour ce s in G O O D S-N at 5.5 G H z ba se d on ul tra -de ep JV L A da ta w ith s ub -ar cs ec re sol ut ion A na lys is of the A G N /SFg cont ent in the 5.5 G H z c ata logue vi a 5 I R c c pl ot s, ha rd X -ra y lum inos ity , q 100 ra di o exc es s and V L B I de te cti ons T he m ajor ity of the sour ce s ar e A G N re la te d (m os tly qua sa r m ode ) dow n to a fe w µ Jy 30% of qua sa r m ode AGNs show a r adi o exc es s, 15% V L B I de te cte d qua sa r m ode AGNs and S F/ hyb ha ve si m ila rst ee p ra di o spe ctr a, ra di o m ode AGNs fl at/ inve rte d spe ctr a In t he sa m e sky ar ea , a 1.4G H z se le cte d sa m pl e at ar cs ec re sol ut ion cont ains a la rge r fra cti on of S F/ hyb and st ee p spe ctr a, but AGNs st ill dom ina te L ooki ng for w ar d for eM E R L IN da ta (L ove ll inc lude d) to expl or e the µ Jy & s ub -Jy sky w ith ~ 50 m as re sol ut ion à trul y re sol ve d & unbi as ed vi ew of A G N & S F pr oc es se sup t o hi gh re ds hi fts in G O O D S-N 76m L ove llX
-ra
y
for
63%
(52/
82)
(X ue + 16 ) (20 AGNs , 9 pa s, 15 S F/ hyb )X
-ra
y
A
GN
if
:
Lx [2 -7 ke V ] > 10 42 er g/ s Lx [0.2 -7 ke V ] > 3× 10 42 er g/ s( for upp limits ) 22% of S F/ hyb cont ains an A G N not se en in IR AGN br ight es tX -ra y sour ce s Lx me d 5× 10 43 er g/ s Lx me d 1.7 ×10 41 er g/ s for pa s & SF/ hybX
-ra
y
AGNs
■
44 Q
M
AGNs
▲
RM
A
G
N
●
SF/
hyb
sys
te
m
s
20/
35 i
n
Q
M
AGNs
3/
15 i
n
R
M
AGNs
6/
27 i
n
SF
/hyb
29
sour
ce
s
[
R adi o A G N re ve le ad by a r adi o exc es s wr tw ha t expe cte d from st ar for m ati on (fr om F IR /ra di o ..) & by V L B I de te cti ons 100 µm for 63% ( 52/ 82) (M agne lli + 13, + 15 ) S 100µ m =1m Jy (3 sigm a) for uppe r limits 1.4 G H z V L A for (82/ 82) (M or ris on+ 10)
