The HMXB Z z connection · Chandra XX Different redshifts, same story • Further support that...
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Chandra XX The HMXB Z-z connection Francesca Fornasini Connecting the metallicity dependence and redshift evolution of HMXBs with F. Civano, M. Kriek, R. Sanders, I. Shivaei, H. Suh, and the MOSDEF survey team
Transcript of The HMXB Z z connection · Chandra XX Different redshifts, same story • Further support that...
Chandra XX
The HMXB Z-z connection
Francesca Fornasini
Connecting the metallicity dependence and redshift evolution of HMXBs
with F. Civano, M. Kriek, R. Sanders, I. Shivaei, H. Suh, and the MOSDEF survey team
Chandra XX
Local LHMXB-SFR correlation
Mineo+2012
Star-forming (high sSFR) galaxies
HMXB dominated
sSFR=SFR/M★
M101
NASA/CXC/JHU
Chandra XX
The little z: LHMXB/SFR evolves with redshift
Lehmer+2016
- - Best fit (βSFR(1+z)δ)- - Theoretical model (Fragos+2013)
Stacking galaxies in the Chandra
Deep Field SouthDriven by metallicity
dependence?
Fragos+2013
X-ray Astronomy 2019F. Fornasini
The big Z: The effect of metallicity on HMXB evolution
High-Z Low-Z
X-ray Astronomy 2019F. Fornasini
The big Z: The effect of metallicity on HMXB evolution
High-Z Low-Z
X-ray Astronomy 2019F. Fornasini
The big Z: The effect of metallicity on HMXB evolution
High-Z Low-Z
X-ray Astronomy 2019F. Fornasini
The big Z: The effect of metallicity on HMXB evolution
High-Z Low-Z
X-ray Astronomy 2019F. Fornasini
The big Z: The effect of metallicity on HMXB evolution
High-Z Low-Z
X-ray Astronomy 2019F. Fornasini
Implications of Z-dependence• In addition to providing insight into models of stellar evolution,
HMXB Z-dependence can also constrain:
• progenitor pathways of GW sources • contribution of HMXBs to the heating/reionization of IGM • contamination of HMXBs to low-LX AGN searches in dwarfs
X-ray Astronomy 2019F. Fornasini
Implications of Z-dependence• In addition to providing insight into models of stellar evolution,
HMXB Z-dependence can also constrain:
• progenitor pathways of GW sources • contribution of HMXBs to the heating/reionization of IGM • contamination of HMXBs to low-LX AGN searches in dwarfs
X-ray Astronomy 2019F. Fornasini
Implications of Z-dependence• In addition to providing insight into models of stellar evolution,
HMXB Z-dependence can also constrain:
• progenitor pathways of GW sources • contribution of HMXBs to the heating/reionization of IGM • contamination of HMXBs to low-LX AGN searches in dwarfs
Mezcua+2016
Chandra XX
Evidence of Z-dependence• Local galaxies exhibit
LX-SFR-Z correlation, but samples may be biased
• Redshift evolution of HMXB relation could be effect of Z-dependence or driven by other factors
log(
L X/S
FR)
12+log(O/H)Brorby+2016
Z proxy for HMXBs
Chandra XX
Is redshift evolution of HMXBs driven by metallicity?
redshift
7.5 8.0 8.5 9.039.0
39.5
40.0
40.5
41.0
7.5 8.0 8.5 9.012+log(O/H)
39.0
39.5
40.0
40.5
41.0
L X/SFR
12+log(O/H)
log(
L X/S
FR)
7.5 8.0 8.5 9.039.0
39.5
40.0
40.5
41.0
7.5 8.0 8.5 9.012+log(O/H)
39.0
39.5
40.0
40.5
41.0
L X/SFR
log(
L X/S
FR)
12+log(O/H)
Chandra XX
The MOSDEF Survey• Rest-frame optical spectra for ~1500 galaxies at
z~2 in fields with deep X-ray data
Chandra XX
Chandra extragalactic surveys
Deep Field South7 Ms (80 day) exposure
Luo+2017
Alexander+2003
Deep Field North2 Ms exposure
Nandra+2015
AEGIS-X800 ks exposure
� Chandra XX
Going deeper with existing data
Individual detections of small number
of objects
Average X-ray properties for large sample
of objects
5"
Chandra XX
The MOSDEF sample• O3N2 Z indicator
• Hα SFR
• Exclude X-ray, IR, and optical AGN
• Chandra PSF<3.5”
• 79 galaxies
• Stacked exposures: 20-50 Ms (200-600 days!)
8.5 9.0 9.5 10.0 10.5 11.0 11.5−1
0
1
2
3
8.5 9.0 9.5 10.0 10.5 11.0 11.5log(Mass) [MSun]
−1
0
1
2
3
log(
SFR
) [M
Sun y
r−1]
sSFR=10−8.8 yr−
1
O/H lower limitO/H upper limit
O/H measurementz~2.3z~1.5
O/H lower limitO/H upper limit
O/H measurementz~2.3z~1.5
8.0 8.2 8.4 8.6 8.812+log(O/H)
logS
FR
logM★
Fornasini+2019
Chandra XX
Redshift evolution consistent with previous studies
Fornasini+2019
0.0 0.5 1.0 1.5 2.0 2.5
39.2
39.4
39.6
39.8
40.0
40.2
0.0 0.5 1.0 1.5 2.0 2.5z
39.2
39.4
39.6
39.8
40.0
40.2
log(
L X/S
FR) [
erg
s−1 /(M
Sun
yr−
1 )]
Total XRBLehmer et al. (2016)Aird et al. (2017)
Lehmer et al. (2010)Mineo et al. (2012)This work: full sampleThis work: high sSFR
8.0 8.2 8.4 8.6 8.812+log(O/H)
Chandra XX
Redshift evolution consistent with previous studies
Fornasini+2019
0.0 0.5 1.0 1.5 2.0 2.5
39.2
39.4
39.6
39.8
40.0
40.2
0.0 0.5 1.0 1.5 2.0 2.5z
39.2
39.4
39.6
39.8
40.0
40.2
log(
L X/S
FR) [
erg
s−1 /(M
Sun y
r−1)]
Total XRB
HMXB only
Lehmer et al. (2016)Aird et al. (2017)
Lehmer et al. (2010)Mineo et al. (2012)This work: full sampleThis work: high sSFR
8.0 8.2 8.4 8.6 8.812+log(O/H)
Chandra XX
• First evidence for Z-dependence at z>0 (97% confidence)• Likely driven by HMXBs rather than LMXBs
HMXBs exhibit Z-dependence at z~2
8.0 8.1 8.2 8.3 8.4 8.5 8.6
39.6
39.8
40.0
40.2
40.4
8.0 8.1 8.2 8.3 8.4 8.5 8.612+log(O/H)
39.6
39.8
40.0
40.2
40.4
log(
L X/S
FR
) [e
rg s
−1/(
MS
un y
r−1 )]
Fragos et al. (2013) modelMadau & Fragos (2017) model
Brorby et al. (2016) z=0 relation
High sSFR: log(sSFR)>−8.8Restricted sSFR: −9.2<log(sSFR)<−8.4
−9.0 −8.9 −8.8 −8.7 −8.6 −8.5log(sSFR) [yr−1]
Fornasini+2019
Chandra XX
8.0 8.2 8.4 8.6 8.8
39.2
39.4
39.6
39.8
40.0
40.2
8.0 8.2 8.4 8.6 8.812+log(O/H)
39.2
39.4
39.6
39.8
40.0
40.2
log
(LX/S
FR
) [e
rg s
−1/(
MS
un y
r−1)]
Fragos et al. (2013) modelMadau & Fragos (2017) model
Brorby et al. (2016) z=0 relation
z=0: Mineo et al. (2012)z=0: Lehmer et al. (2010)z~2: Metallicity binningz~2: All high sSFR
• HMXB-only normalization consistent with z=0 relationFornasini+2019
The Z-z connection
Chandra XX
Evidence favors Z-z connection
• But is the local LX-SFR-Z relation biased?
• Can we improve measurements of this relation to provide better constraints for theoretical models?
Chandra XX
Civano+2016 COSMOS 160 ks exposure per
pointing
Studying Z dependence at low z
Galaxy information from two spectroscopic surveys:hCOSMOS (z=0.1-0.4)zCOSMOS (z=0.5-0.9)
Chandra XX
Studying Z dependence at low z
Fornasini+in prep
• hCOSMOS sample: 858 galaxies at z=0.1-0.4
• zCOSMOS sample: 787 galaxies at z=0.5-0.9
• R23 Z indicator
• SED (UV+IR) SFR
• Exclude X-ray, IR, and optical AGN
0.0 0.5 1.0 1.5 2.0 2.5Redshift
39.2
39.4
39.6
39.8
40.0
40.2
log(
L X/S
FR) [
erg
s−1 /(M
Sun
yr−
1 )]
Aird et al. (2017)Lehmer et al. (2016)
Lehmer et al. (2010)Mineo et al. (2012)Fornasini et al. (2019)This work
8.1 8.3 8.5 8.7 8.9log(O/H)+12
Chandra XX
Different redshifts, same story
• Further support that z-evolution driven by metallicity• Theoretical models with high LX/SFR are in
disagreement but SFR systematics are important
8.0 8.2 8.4 8.6 8.839.039.2
39.4
39.6
39.8
40.0
40.2
40.4
8.0 8.2 8.4 8.6 8.812+log(O/H)
39.039.2
39.4
39.6
39.8
40.0
40.2
40.4lo
g(L X
/SFR
) [er
g s−
1 /(MSu
n yr−1
)]Fragos et al. (2013) model
Madau & Fragos (2017) modelBrorby et al. (2016) z=0 relation
z=1.3−2.7: Fornasini et al. (2019)z=0.5−0.9: zCOSMOS (this work)z=0.25−0.4: hCOSMOS (this work)z=0.1−0.25: hCOSMOS (this work)z=0: Mineo et al. (2012)z=0: Lehmer et al. (2010)
Fornasini+in prep
Chandra XX
• We have measured the HMXB Z-dependence at z>0.
• Z-dependence at different redshifts is consistent and accounts for the observed z-evolution of LHMXB/SFR
The Z-z connection: summary & outlook
Larger spectroscopic
samples
Improved SFR estimates
Larger, deeper X-ray surveys
+
hCOSMOS+ survey
![Probing dark matter halos at redshifts z=[1,3] with lensing magnification](https://static.fdocuments.in/doc/165x107/568158e4550346895dc62659/probing-dark-matter-halos-at-redshifts-z13-with-lensing-magnification.jpg)
