Hunting Axion Dark Metter with
Protoplanetary Disk Polarimetry/31/“)()”@, 2018/12/19-21

Cygnus A

6000
2000

4000

GRB 110301A0Count rate (counts/s)

The Astrophysical Journal Letters, 758:L1 (5pp), 2012 October 10

Figure 4

3000

GRB 110721A

2000

Count rate (counts/s)

Comparison of radio (red), X-ray (blue), and optical images of the Cygnus A FR-II radio galaxy(center). While the X-ray traces primarily hot old cocoon emission and the radio traces the jetand new cocoon emission, the three primary hot spots are bright in both energy bands with asynchrotron peak in the radio and a Compton scattering peak in the X-ray. The nearly-symmetricblack hole jet is shown at bottom, with a scale 20,000 times smaller than the larger image. Credit:
X-ray: NASA/CXC/SAO; Optical: NASA/STScI; Radio: NSF/NRAO/AUI/VLA; VLBI inset:
Boccardi et al. (2017).

01000

In a radio flux density-limited sample of flat-spectrum AGN selected at 5 GHz it was
found that only ⇠ 20% of the objects are detected inrays (Karouzos et al. 2011). However
all of the Fermi-detected blazars north of declination 20 are detected in the OVRO 40m Telescope monitoring campaign Richards et al. (2011). Karouzos et al. (2011) find nostrong link between fast apparent speeds andray detectability, as measured with Fermi.
They argue that this is evidence for a “spine-sheath” structure (Sol et al 1989; Laing 1996)
in which the outer layers of the relativistic jet, which form the “sheath” have slower bulk
velocity along the jet axis than do the inner layers, which form the “spine”. Such a structure
01020could also explain the relative fractions of AGN that are
ray bright and radio bright, if
Time since GRB trigger (second)
the spine is predominantly
ray-emitting and the sheath is predominantly radio-emitting.
In a comprehensive review ofray observations of AGN, Madejski & Sikora (2016)
Figure 1. Light curves of the prompt gamma-ray emission of GRB 110301A
found that theray flux density variations in blazars show generally greater fractional(top) and GRB 110721A (bottom) detected by GAP. The vertical dashed lines
amplitudes than the other observed bands, and stronger flares tend to occur when the flux
indicatefrom
theseveral
time interval of polarization analyses for each burst.
density is at a higher-than-average level, with the activity lasting anywhere

Yonetoku, Murakami, Gunji, Mihara, KT+2012;
Boccardi+2017; Blandford+2018• • 

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bound on j"j would be tighter. Without
nature of the intrinsic polarization of the sothe one that"CPT!
gives the weakest bound on j"j amdo not exhibit the accidental cancellation me
For GRB 110721A, the 2& lower limits %$ > 35% in the whole energy band (E⇠ keV.
Emax ¼ 300 keV) leadtoE’120!± ' k2±k 2 Se
plin j#!ðE2 ; zÞ " #!ðEmin ; zÞj ) M#=2,
we ostraint from GRB 110721A as j"j < 7 ( 10More accurate
constraints are obtain• "pﬃﬃﬃﬃﬃﬃﬃﬃﬃﬃﬃﬃﬃﬃﬃﬃﬃ
ﬃ
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   
Q ¼ Emin E $i cos½2#!ðE;zÞ', and U ¼
"sin ½2#!ðE; zÞ' with the intrinsic polari$i ¼ 1. Using •$P(70-300keV)> 0:35 and> %>(2s)"0:98,35%
constraint from GRB
110721A as(D > 2.5Gpc)
for GRB110721A<latexit sha1_base64="(null)">(null)</latexit>

KT, Mukohyama, Yonetoku et al. 2012;
Myers & Pospelov 2003

j"j < 2 ( 10"15 ;g, (t) is the background field value of the ADM
denotes the time derivative. Here, we chose theal gauge A0 = 0 and the Coulomb gauge r·A = 0.
g the cosmic expansion, the present backgroundlike particles by(ALPs)
eld•isAxion
well approximated

Axion dark matter scenario(t) =0 cos(mt +),(2)⇢DM = m750(c T /10and hence
So far, w
coherently
factor .
wavelengthe constant amplitude 0 , the axion mass m and a1 ˙2
mof theHrec ⇠ 10 27 eV
hP i =thath (the spatialm2 2 )idependence!0actor . Note2
actor (x) will be discussed later.
1) canif one decomposesthe DM)i into•  be reduced
(waveAor“fuzzy”
with v3 ⌘polarization
modes
intheFourier
space,
ØCore-cusp problem, satellite problem etc.
show a cohZ3X
d k p
2p
ik·x
assume th~GM~
Ai (t, x) =r ⇠A(t)e(k̂)e,(3)ir >> 3 k(2⇡)
2value in e
GM m2
mvp=± v✓◆2 tha
922 longer
10 M
10eVp⇤
p' 0.1
kpc
veci (k̂) = ei ( k̂) is the circular polarization
MmHu, Barkana & Gruzinov
2000;
&0p
⇤p0 Schive, Chiuehpp±
Ostriker,(Tremaine2017 ✏ijm kj em (k̂) =chBroadhurst
obeys2014;
ei Hui,(k̂)ek̂) = & Witten, andi<latexit sha1_base64="(null)">(null)</latexit><latexit sha1_base64="(null)">(null)</latexit><latexit sha1_base64="(null)">(null)</latexit><latexit sha1_base64="(null)">(null)</latexit><latexit sha1_base64="(null)">(null)</latexit>

under discussion [13].

Axion-photon
coupling
eviousworks attempted
to test the ultraith m ⇠ 10 22 eV by using the coupling beand photon, La = ga Fµ⌫ F̃ µ⌫ /4. This
edicts two di↵erent phenomena: One is the2particle and ˙a photon untween anÄaxionr Ai = gg (t)✏ijk @j Ak
ifields, and the other is the photon birefrinaxion background. Exploiting the former
axion •helioscope[14, 15] and conversion“light shinPrimakoff axion-photon φA searching
a wall” experiments[16] arefor
physical observations of SN1987A [17] and• Birefringence
were also φstudiedto detect the signatures
A 
sion. However, no signal is yet to be ob<latexit sha1_base64="(null)">(null)</latexit>

Caroll, Field & Jackiw 1990

e1
1
i tt+T !dt
e ±kei (k̂). Then+Eq.
e (1) reads
ii
2
2 ±
R t+T
Ä!±+!
(± Ak = 0 ,kcos( t! dt)
ikTR=e.
(7)
withsin( t+T ! dt)
t11˙!
'k±!,!
⌘ga 0 msin(mt+ ), (!
'k±ga ±The±rotation angle
ofthelinear
polarization
planeis22
given by⌘ ! k | !|. Therefore under the oscillawhere we assume
Z t+Ting
axion background, the dispersion relation of photon✓(t, T ) = modified!(t)and dtthe, phase velocities of the left/right-handetmodes
are di↵erent. This is because theparity symmetr
12 ✓◆✓+ ⌅ + ) g m◆
1⇡ 2is⇥spontaneously
10 sin mT⌅ sin(mt,field.
(8)12This12axion
22brokenbythephotomTg/10GeVa⇡ 2 ⇥ 10 2 sin
sin mt ++22 eVleads
birefringencecausedbytheaxion
background
22m/10122
where g12 ⌘thega rotation/(10 12 GeV),m⌘m/(10eV)
22of the linear polarization plane.
and we used Provided
the darkthat
matterdensityaround alongus, the z-ax
aphotonpropagating• $ %#23⇢DM = m2 is/2⇡
0.3
GeV/cm[22].
⌅⌘ mT /2 its⇡ polarizatio
0 linearly polarized into
thex-direction,•  &   ! 750(c T /100pc)mmuch
larger into
thantheunity22 is typicallycomponents
canbedecomposed
circularones,~•and$%#"
22
hence the factor sin ⌅✓is expectedbe ⇠O(1).
1.3/(m/10eV) yr◆ tp ⇠✓ to ◆✓◆2
1 axion11mc background1
So far, we have considered1 thatthe=+,(0ii
2 a constant2
Fujita,Tazaki & KT 2018,arXiv:1811.03525
coherently
oscillates
everywhere with
phase
it+T
± !dttBirefringence<latexit sha1_base64="(null)">(null)</latexit><latexit sha1_base64="(null)">(null)</latexit><latexit sha1_base64="(null)">(null)</latexit><latexit sha1_base64="(null)">(null)</latexit>1. Itlength;therefore,scatteredAB
lightis expected
to aristionoftheobject,
Aur,performed
byllates
the samecoherent
axion
field.
Protoplanetarydiskpolarization
al.
[26]
presents
ausefuldata to assess theecan)
At Theynear-infrared
wavelengths,
a numberof polari
showedthatahistogramofpolarizati
n po-ric imaging observations of PPD have been perform
to radial vectors can be fitted by a G
s alsoTheserespectobservations have demonstrated that observedtion with central position of 90 .1 ± 0 .2 a↵ects.larimetricpattern is consistent with disk scattered.
4 .3 + 0 .4. Within the 1 accuracy, pointerpretation [e.g. 26, 28]. Among these, an obsetgles
areconsistentwiththoseofscatteredtion of the object, AB Aur, performed by Hashimot
swords,rotation
ofdatapolarization
anglesdual.
[26]
presents
ausefultoassessthebirefringe
1″nfieldshouldbeless than
0 .3 for 1 angles, whicTheyshowedthatahistogramofpolarization
80859095100
3Angle (degree)
toto5 radial⇥ 10 vectors
radian.
Therefore,
thecurrenfarporespectcanbe
fittedbyaGaussiano• AB Aurigae (cT = 162.9 pc)
ontherotation
angle✓
causedbytheAD
tized
tion
with
centralposition
of
90
.1
±0.2
andFWH3.
mT/2 ~ 10 >> 1.3 + 0HiCHAO.4. Within
the 1 accuracy, polarization
ne ro-•4 Subaru(near IR)
3|✓|<5⇥
10, In ogles
areconsistentwiththoseofscattered
light.
eitherspeed of the spiral structure is given by
resence of unseen planets in the disk can also result

Hashim0Number
200
400600ophysical Journal Letters, 729:L17 (6pp), 2011 March 10Polarization vector pattern of AB Aur. Left: polarization vectors superposed on the PI image of AB Aur in the H band. The plotted vectors arl binning which corresponds to the spatial resolution and have a polarized intensity larger than 50σ . Not all the vectors are plotted and their lengr the purposes of presentation. Right: histogram of angles between polarization vectors and lines from the mask center to the vector position. Asfitting, the central position and FWHM are 90.◦ 1± 0.◦ 2 and 4.◦ 3± 0.◦ 4, respectively.
ersion of this figure is available in the online journal.)

Hashimoto+2011 over the disk scale even in thebations
which extend!
"duewords, rotation of polarization angles
tothe a$#13

Upper limit on gag from PPD pol.

tized plasmas and[24, 25], those dee↵ect as we showeof purely scattere
only optical andwell-observed PP
regions in our Gtances. Then in o(or detect) the A
keep increasing tments of PPDs.

9CAST10log10 (ga /GeV 1 )SN 1987A

11Quasor polarization

1213ALPS-IIIAXOSoft X-ray
ray transparency
This work

14

1525

24

23

22

21
20
19
log10 (m/GeV)

18

17

16

15

ACFIG. 1: Constraint on the coupling constant ga for varying-21the axion dark matter m. The solid line indicates
We are gratefu
mass ofthe upper bound derived in eq. (14). Blue, green, and redworkshop ‘Essent
regions are rejected by the experiment (CAST [14]) and asogy’ held on June
tronomical observations (SN 1987A [17] and QuasorFujita,
polarizaTazaki & KT
2018,
Dias+2014
sity,wherewe ction [18]). Black broken lines are the expected sensitivities• m < 10 eV 



Summary & Discussion• Axion dark matter• m  10-22 eV (for a solution of the structure formation problems)• Oscillating scalar field φ(t)• >(axion!" 3<K>4 ): 
• -7EDA*G$1DIF>K>4 '1*;# axion?9B
• .9@H/6m < 10-21eVgag,C %=• 50J&8+K>@H 2

• For more details, see Fujita, Tazaki & Toma, arXiv:1811.03525• See also Ivanov+2018 for a constraint from AGN jet pol., and Sigl & Trivedi 2018(and references therein) from CMB pol.

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