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CW signals Directed searches O2 GC O3 new sources
Searching for continuous gravitational-wavesfrom Galactic neutron stars
Ornella Juliana Piccinni for the Rome CW groupAstone P., D’Antonio S., Frasca S., Intini G., Leaci P.,
Mastrogiovanni S., Miller A., Palomba C., La Rosa I.
University of Rome ’Sapienza’ & INFN Roma1
September 26, 2019
YITP workshop 2019 September 26, 2019 0 / 16
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CW signals Directed searches O2 GC O3 new sources
Overview
Intro on Continuous waves signals
Focus on directed searches
The Galactic Center O2 case
New sources from Fermi and Integral catalogs for O3
YITP workshop 2019 September 26, 2019 1 / 16
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CW signals Directed searches O2 GC O3 new sources
Gravitational waves sources
Modeled waveform Unknown waveform
Long-lived
Transients
YITP workshop 2019 September 26, 2019 2 / 16
T ∼ monthsor years
T ∼ up to100 s
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CW signals Directed searches O2 GC O3 new sources
Gravitational waves sources
Modeled waveform Unknown waveform
Long-lived
Transients
YITP workshop 2019 September 26, 2019 2 / 16
T ∼ monthsor years
T ∼ up to100 s
Compact binary coalescenceh0 ∼ 10−21
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CW signals Directed searches O2 GC O3 new sources
Gravitational waves sources
Modeled waveform Unknown waveform
Long-lived
Transients
YITP workshop 2019 September 26, 2019 2 / 16
T ∼ monthsor years
T ∼ up to100 s
Compact binary coalescenceh0 ∼ 10−21
Bursth0 ∼ 10−21
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CW signals Directed searches O2 GC O3 new sources
Gravitational waves sources
Modeled waveform Unknown waveform
Long-lived
Transients
YITP workshop 2019 September 26, 2019 2 / 16
T ∼ monthsor years
T ∼ up to100 s
Stochastic backgroundh0 ∼ 10−28
Compact binary coalescenceh0 ∼ 10−21
Bursth0 ∼ 10−21
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CW signals Directed searches O2 GC O3 new sources
Gravitational waves sources
Modeled waveform Unknown waveform
Long-lived
Transients
YITP workshop 2019 September 26, 2019 2 / 16
T ∼ monthsor years
T ∼ up to100 s
Continuous wavesh0 ∼ 10−25
Stochastic backgroundh0 ∼ 10−28
Compact binary coalescenceh0 ∼ 10−21
Bursth0 ∼ 10−21
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CW signals Directed searches O2 GC O3 new sources
Gravitational waves sources
Modeled waveform Unknown waveform
Long-lived
Transients
YITP workshop 2019 September 26, 2019 2 / 16
T ∼ monthsor years
T ∼ up to100 s
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CW signals Directed searches O2 GC O3 new sources
What is a Continuous Wave (CW)?
Credit: C. Reed, Penn State/Mc Gill University
Persistent signal (long-lived)
Produced by a nearly periodic mass quadrupole moment variation
Expected sources
Isolated neutron stars (NS) or NSs in binary systems (Non-axisymmetric)
Expected strain
h0 ∼= 10−27(
Izz1038kg·m2
)(10kpcd
)(f
100Hz
)2 (�
10−6
)� h0CBC
[For a CW review: Lasky PASA 32, pp. 34 (2015), Riles Mod Phys Lett A 32, No. 39, 1730035 (2017)]
YITP workshop 2019 September 26, 2019 3 / 16
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CW signals Directed searches O2 GC O3 new sources
Isolated neutron stars
Credit: S. Mastrogiovanni
h0 =4π2Gc4
Izzf2
d �Izz: moment of inertia�: ellipticity
YITP workshop 2019 September 26, 2019 4 / 16
The signal is modulated: Doppler effect, spin-down, sidereal day variation,antenna response, etc.
The ellipticity can be triggered by different factors: elastic stress, stronginternal magnetic fields, thermal gradients, etc. Lasky PASA 32, pp. 34 (2015)
The maximum ellipticity that a neutron star can sustain is related to theequation of state and to the neutron stare interior model (Johnson-McDaniel+ PRD 88,044004 (2013))
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CW signals Directed searches O2 GC O3 new sources
Estimates on �
Theoretical models (K. Glampedakis & L. Gualtieri 2018 [Astro. and Space Science Lib., vol457. Springer])
Solid strange stars: � 6 6× 10−4
Hybrid and meson condensates stars: � 6 3− 9× 10−6
Canonical magnetic deformations: � 6 2− 6× 10−7
Buried magnetic field in MSPs: �fid ∼ 10−9 and a buriedmagnetic field of 1011 G G. Woan+[ApJL,863:L40, 2018]
These are even more stringent than (Johnson-McDaniel+ PRD 88, 044004 (2013))
� ≤ 10−5 normal NS
� ≤ 10−3 hybrid stars
� ≤ 10−1 extreme quark stars
YITP workshop 2019 September 26, 2019 5 / 16
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CW signals Directed searches O2 GC O3 new sources
Directed searches so far
In directed searches interesting sky regions or astrophysical objectsare investigated:
O1: 15 SNR + Fomalhaut b (LVC, ApJ 875 122, 2019)
O1: LMXB Scorpius X-1 (LVC, ApJ 847 47, 2017)
O1: Terzan 5 and the galactic center (Dergachev et al.arXiv:1903.02389)
O1: Vela Jr., Cassiopeia A and G347.3 (Ming et al.arXiv:1903.09119)
Other (LIGO S6): the Orion Spur, NGC 6544, LMXB XTEJ1751-305
Coherent or incoherent methods can be used
YITP workshop 2019 September 26, 2019 6 / 16
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CW signals Directed searches O2 GC O3 new sources
BSD directed search pipeline
BSD time series(Piccinni+ CQG 36, 015008, 2019)
2.30465 2.3047 2.30475 2.3048 2.30485 2.3049 2.30495
time (s) 10 6
-6
-4
-2
0
2
4
6
10-3 TIme series
Partial Dopplercorrection
Time-frequency peaks(Astone+ CQG 22, S1197, 2005)
YITP workshop 2019 September 26, 2019 7 / 16
Frequency Hough map(Astone+ PRD 90, 042002, 2014)
The most significant candidates are selected onthe final HM. The total computational power
needed for this search is ∼ 100 CPU hours pertarget for a ”wide” frequency/spin-down range
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CW signals Directed searches O2 GC O3 new sources
Motivation for a Galactic center search
Several independent lines of evidence predict a sizable population ofneutron stars in the region (O(108 − 109) expected in the fullGalaxy, only a fraction observed)
Given the large number of massive stars, the central parsec likelyhosts a large neutron star population (mostly MSP (Macquart, J.P. et al.2015))
A GC pulsar population could explain the Galactic Center GeV excessmeasured by Fermi (Bartels et al. 2016, Lee et al. 2016, Fermi-LAT coll. 2017)
The size of the potentially EM observable population (i.e. thosebeaming towards us) could include up to 50 canonical pulsars and10000 millisecond pulsars (Rajwade et al. 2016)
The Galactic center is a good place to look for CWssince it is likely to host several candidates
YITP workshop 2019 September 26, 2019 8 / 16
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CW signals Directed searches O2 GC O3 new sources
Motivation for a Galactic center search
Several independent lines of evidence predict a sizable population ofneutron stars in the region (O(108 − 109) expected in the fullGalaxy, only a fraction observed)
Given the large number of massive stars, the central parsec likelyhosts a large neutron star population (mostly MSP (Macquart, J.P. et al.2015))
A GC pulsar population could explain the Galactic Center GeV excessmeasured by Fermi (Bartels et al. 2016, Lee et al. 2016, Fermi-LAT coll. 2017)
The size of the potentially EM observable population (i.e. thosebeaming towards us) could include up to 50 canonical pulsars and10000 millisecond pulsars (Rajwade et al. 2016)
The Galactic center is a good place to look for CWssince it is likely to host several candidates
YITP workshop 2019 September 26, 2019 8 / 16
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CW signals Directed searches O2 GC O3 new sources
The Galactic center case: O2
Best results h01.4× 10−25 for L @ 163 Hz, 1.6× 10−25 for H @ 195 Hz at 95% C.L.
10 1 10 2
Frequency [Hz]
10 -25
10 -24
10 -23
10 -22
10 -21
h95
%0
H 95% C.L.L 95% C.L.
YITP workshop 2019 September 26, 2019 9 / 16
Frequency: [10, 710] Hz
Spin-down: [−1.8 × 10−9, 3.7 × 10−11] Hz/s
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CW signals Directed searches O2 GC O3 new sources
The Galactic center case: O2
Since h0 ∝ Izzd �f2 → � = c
4
4π2G
(dIzz
)h0f2
d=8 kpc and a moment of inertia Izz = Ifid = 1038 kg m2 for standard
NSs or 5 times larger for more exotic objects
0 100 200 300 400 500 600 700Frequency [Hz]
10 -6
10 -4
10 -2
10 0
10 2
95 %
H, Ifid
L, Ifid
H, 5Ifid
L, 5Ifid
YITP workshop 2019 September 26, 2019 9 / 16
� ≤ 10−5 normal NS� ≤ 10−3 hybrid stars� ≤ 10−1 extreme quark stars(Johnson-McDaniel+ PRD 88, 044004 (2013))
We can exclude the presence ofstars with ellipticity bigger than10−6 in the GC region at thehighest frequency
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CW signals Directed searches O2 GC O3 new sources
Other potential sources
Sources which are likely hosting a NS are interesting candidates forour searches.
Several potential sources are present in the astronomical catalogslike:
the pre-release of the 8-years Fermi-LAT point sources catalog1:identified or associated Supernova remnants or Pulsar Wind Nebulaor unassociated sources (∼ 39%)
1https://fermi.gsfc.nasa.gov/ssc/data/access/lat/fl8y/YITP workshop 2019 September 26, 2019 10 / 16
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CW signals Directed searches O2 GC O3 new sources
Fermi-LAT unassociated
Unassociated: 2132 in Fermi-LAT (∼ 39%) we have only gamma-raysobservation, no counterparts at other wavelengths
0 50 100 150 200 250 300 350 400
(o)
-100
-50
0
50
100
(o)
unassociatedGC
YITP workshop 2019 September 26, 2019 11 / 16
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CW signals Directed searches O2 GC O3 new sources
Other potential sources
Sources which are likely hosting a NS are interesting candidates forour searches.
Several potential sources are present in the astronomical catalogslike:
the pre-release of the 8-years Fermi-LAT point sources catalog2:identified or associated Supernova remnants or Pulsar Wind Nebulaor unassociated sources (∼ 39%)
the IBIS-INTEGRAL soft gamma-ray source catalog (Bird+ 2016):10 SNR, 19 pulsar-like sources and 216 unidentified ones (23%)
2https://fermi.gsfc.nasa.gov/ssc/data/access/lat/fl8y/YITP workshop 2019 September 26, 2019 11 / 16
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CW signals Directed searches O2 GC O3 new sources
IBIS-INTEGRAL
INTEGRAL catalog presents the following interesting sources: 10 SNR,19 pulsar-like sources and 216 unidentified ones (23%) which skydistribution is shown below:
0 50 100 150 200 250 300 350 400
( o )
-100
-80
-60
-40
-20
0
20
40
60
80
100
(o)
unidentifiedbinariesGCPSR+SNR+
YITP workshop 2019 September 26, 2019 12 / 16
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CW signals Directed searches O2 GC O3 new sources
Other potential sources
Sources which are likely hosting a NS are interesting candidates forour searches.
Several potential sources are present in the astronomical catalogslike:
the pre-release of the 8-years Fermi-LAT point sources catalog3:identified or associated Supernova remnants or Pulsar Wind Nebulaor unassociated sources (∼ 39%)
the IBIS-INTEGRAL soft gamma-ray source catalog (Bird+ 2016):10 SNR, 19 pulsar-like sources and 216 unidentified ones (23%)
Most of the sources lie on the Galactic plane
3https://fermi.gsfc.nasa.gov/ssc/data/access/lat/fl8y/YITP workshop 2019 September 26, 2019 12 / 16
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CW signals Directed searches O2 GC O3 new sources
How good is a target
For a given pipeline we can have an estimate of the search sensitivity
(Astone+ 2014) as h0min ≈√Sn(f)
α (minimum detectable GWstrain amplitude)
For directed searches we use the age based upper limit hage forthose sources whose age and distance is known (Wette 2008)
A good target will have hage > h0min
All these quantities can be translated in terms of the star ellipticity�age and �min
YITP workshop 2019 September 26, 2019 13 / 16
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CW signals Directed searches O2 GC O3 new sources
Theoretical indirect upper limits: O3
Potentially detectable sources by our directed search pipeline, with hagebigger than our search sensitivity.
YITP workshop 2019 September 26, 2019 14 / 16
hage 6 1d
√5GIzz8c3τ
h0min ≈√Sn(f)
α
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CW signals Directed searches O2 GC O3 new sources
Theoretical indirect upper limits on the ellipticity
Since h0 ∝ Izzd �f2 → �min = c
4
4π2G
(dIzz
)h0minf2
�min at 95 % C.L. for Avanced LIGOand Advanced Virgo at designsensitivity for sources at d = 1 kpc and20 kpc The �age theoretical indirectupper limit is
�age ≤√
5c5
128π4GIzzτf4
YITP workshop 2019 September 26, 2019 15 / 16
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CW signals Directed searches O2 GC O3 new sources Conclusion
Conclusion
CW could be the next surprise in GW astronomy given the enhancedsensitivity of the detectors along with the development of newpipelines
Astronomical catalogs (Fermi, INTEGRAL,...) provide good targetsfor our searches, EM observation are crucial
We plan to analyze O3 data looking for sources from the Galacticcenter plus other targets
A CW detection will provide information on the quadrupolardeformation (ellipticity)
With a joint CW and EM observation we can measure NS radius,mass, magnetic field and ellipticity ⇒ EOS
YITP workshop 2019 September 26, 2019 16 / 16
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CW signals Directed searches O2 GC O3 new sources Conclusion
YITP workshop 2019 September 26, 2019 16 / 16
Thank you!
CW signalsDirected searchesO2 GCO3 new sourcesâ•¢Conclusion
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