ear The NASA–ESA mission LISA will measure gravitational ...s ! ear e i e Offie y g Oct 2020*:...
Transcript of ear The NASA–ESA mission LISA will measure gravitational ...s ! ear e i e Offie y g Oct 2020*:...
LISA’s !rst yearPromises and Challenges of LISA ScienceMichele Vallisnerifor the LISA Mission Science OfficeJet Propulsion Laboratorylisa.nasa.gov www.lisascience.org
Oct 2020*: launch!
Jan 2022: acquire & calibrate
cruise (14 months)
1 Apr 2022: begin science operation end year 1 (four more years!)
Massive black-hole binaries• study the galaxy-MBH coevolution• measure accurate distances of high-z
objects to determine cosmology• test GR in the nonlinear regime
Challenge: produce accurate, efficient inspiral–merger–ringdown templates
National Space and Aeronautics Administration
The NASA–ESA mission LISA will measure gravitational waves with frequencies of 0.1 mHz–0.1 Hz. LISA sources include massive-BH mergers, the inspirals of compact objects into central galactic BHs, the binaries of compact stars in our Galaxy, and possibly GW relics from the Big Bang.
The three LISA spacecraft orbit the Sun in a 5-million-km triangular formation. LISA measures GWs using laser interferometry to monitor the distance !uctuations between freely falling test masses, which are protected from external disturbances by the drag-free control of the spacecraft.
day 1–day 365: 23,000 detections of known and and unknown Galactic binaries
RX J0
806.3
HP
Lib
AM C
Vn
EI P
sc
V803
Cen
V407
Vul
ES C
et
������ ���������� �� �� ���� ������ ���� ���������� ������������������ ���� ���� �� �� ������������ �� �� �� ���� �� �� �� ������ �� �� ���� ��
at least 6 known AM CVn’s and one cataclysmic variable
150
59 previously undetected mass-transferring systems; 248 after Galactic foreground subtraction
9,816 previously undetected detached systems (173 on day 1); 22,643 after foreground subtraction
day 10–day 365: 122 detections of extreme mass-ratio inspirals
day 2–day 363: 39 detections of massive and intermediate-mass black-hole binary coalescences
z�0
z�15
�1�106�5�
104 �M �
,z�2.,SNR�190
�4�105�1�
104 �M �
,z�4.6,SN
R�125
�2�104�8�
103 �M �
,z�6.9,SN
R�134
�1�104�1�
103 �M �
,z�9.1,SN
R�40
�4�103�5�
102 �M �
,z�8.1,SN
R�21
�5�103�2�
102 �M �
,z�3.9,SN
R�12
�1�103�4�
102 �M �
,z�12.,SN
R�10
�2�103�2�
103 �M �
,z�15.,SN
R�21
�2�104�9�
103 �M �
,z�5.7,SN
R�184
�4�104�1�
103 �M �
,z�5.,SNR�88
�3�107�3�
105 �M �
,z�1.,SNR�103
�2�105�1�
104 �M �
,z�1.7,SN
R�742
�2�104�5�
103 �M �
,z�2.7,SN
R�188
�2�103�1�
103 �M �
,z�10.,SN
R�23
�1�103�5�
102 �M �
,z�9.7,SN
R�13
�2�103�5�
102 �M �
,z�5.1,SN
R�19
�3�106�5�
103 �M �
,z�1.6,SN
R�52
�1�104�1�
104 �M �
,z�8.7,SN
R�122
�8�104�3�
103 �M �
,z�9.,SNR�114
�2�104�2�
102 �M �
,z�8.6,SN
R�19
�1�103�4�
102 �M �
,z�8.7,SN
R�11
�2�104�1�
104 �M �
,z�7.9,SN
R�167
�3�103�5�
102 �M �
,z�11.,SN
R�17
�3�105�1�
103 �M �
,z�5.1,SN
R�55
�2�103�9�
102 �M �
,z�12.,SN
R�18
�8�104�5�
104 �M �
,z�4.2,SN
R�601
�5�103�2�
103 �M �
,z�7.8,SN
R�41
�1�106�6�
103 �M �
,z�7.1,SN
R�16
�1�105�5�
103 �M �
,z�6.1,SN
R�189
�7�103�5�
103 �M �
,z�6.1,SN
R�87
�1�105�9�
102 �M �
,z�9.9,SN
R�37
�6�103�1�
103 �M �
,z�9.3,SN
R�34
�8�104�5�
103 �M �
,z�4.6,SN
R�222
�5�105�2�
104 �M �
,z�1.1,SN
R�1234
�9�104�5�
104 �M �
,z�7.2,SN
R�369
�1�104�8�
102 �M �
,z�9.2,SN
R�36
�5�104�2�
102 �M �
,z�7.6,SN
R�26
�7�103�2�
102 �M �
,z�12.,SN
R�12
�1�103�8�
102 �M �
,z�12.,SN
R�15
dots show merger events;lines begin at confirmedinspiral detections30% systems are located to 10 deg2 and 10% DL
results for merger-tree population with light seeds and efficientaccretion fromArun et al. (2009)
results for SDSS-calibrated Galactic binary population with He-starmass-transferring systems fromNissanke et al. (2011)detected sources are subtractedfrom the dataset, resulting ina much lower confusion foreground
several more known systems have uncertain GW luminosities or will be detected in the next four years
Galactic binaries• study the astrophysics of binary
stellar evolution, including the common envelope phase
Challenge: design the probabilisticrepresentation and querying of the source catalog
Extreme mass-ratio inspirals• study MBHs and their environment
in the dense nuclei of galaxies• map BH spacetimes, test no-hair
theorem and cosmic censorship
Challenge: develop accurate and efficient signal templates
Cosmic-string bursts and stochastic backgrounds• look for new physics from
the early Universe and string theory
Challenge: characterize space of models and theories
�� �� �� �� �� ���� ���� �� ���� �� �� ���
��� �� �������
������� �������������� �
�
���� �� ���
� ���� ���� �� ���� �� ����
�������������
�����
���������� �� �
��� ����
���������� ��
������������
������ ����
����
���� ��������
���� ���
� �� ���� ��
������ ��
���� �
�����
������
������
���������
� �������� �� �������� �
�
������
–5 –4 –3 –2 –1 0
–20
–19
–18
–17
–24
–23
–22
–21
–20–16
–19–15
veri!cationbinaries
galactic binaryforeground
106+106 M BH–BH at z=1(last 3 years)
log10 f/Hz
LISA sensitivity to monochrom
atic sources(strain needed for SNR=1 in 1 yr ): log
10 hLISA
inst
rum
ent n
oise
: log
10 "
S n /Hz–1
/2
105+105 M BH–BH at z=1(last 3 years)
instrumentnoise
best estimatefor LISA Path!nder
10+106 M EMRI at 3 Gpc(last 3 years)
the LISA sensitivity
z�0
z�1
histogram of detections/day
detection rate out to z = 1 from LISAscience requirement document (2010)
10!42
10!40
10!38
10!36
10!34 !resolved systems: detached mass-transferring
10!4 10!3 10!2inst
rum
ent &
con
fusio
n no
ise:
S n [Hz–1
]
f [Hz]
confusion foreground: unsubtracted subtracted
instrument noise