Cosmological Principle The CDM: successful concordance model of - - PowerPoint PPT Presentation

COSMIC ANISOTROPIES FROM QUASARS

Anisotropies co(s)miques avec les quasars

VINCENT PELGRIMS

– Dautreppe 2018 Dernière Nouvelles de l’Univers –

Grenoble, Décembre 6, 2018

2

• V. Pelgrims

Cosmological Principle

Cosmological principle + General Relatjvity → FLRW Universes [e.g Trodden & Carroll 2004]

[Planck 2013 XV]

The ΛCDM: successful concordance model of cosmology

Though, some anomalies:

• Low-l defjcit in the TT angular power spectrum
• Small temperature variance
• Dipole and quadrupole alignment of moments
• Excess of Integrated Sachs-Wolfe efgect signal
• ...
• Departure from isotropic H0 from SNIa
• Extreme-scale alignments of quasar

(optjcal) polarizatjon vectors

• …

3

• V. Pelgrims

Cosmological Principle

The Universe has to be homogeneous and isotropic when it is viewed at suffjciently large scale. It requires/implies that the part of the Universe that we observe and study is a statjstjcally representatjve sample of its entjrety.

[Planck 2013 XV]

➢ Isotropy for all observers implies homogeneity ➢ Homogeneity for all does not imply isotropy ➢ Bianchi cosmological models that are homogeneous and anisotropic

Resurgent interests to explain some anomalies such as:

• Low-l defjcit in the TT angular power spectrum
• Small temperature variance
• Dipole and quadrupole alignment of moments
• Excess of Integrated Sachs-Wolfe efgect signal
• ...
• Departure from isotropic H0 from SNIa
• Extreme-scale alignments of quasar

(optjcal) polarizatjon vectors

• …

Isotropy appears to be questjonable …

➢ Homogeneity = same observatjon can be made from wherever ➢ Isotropy = same observatjon can be made by looking in whatever directjon

4

• V. Pelgrims

Cosmological Principle

[Springel et al. 2005]

Isotropy appears to be questjonable … Homogeneity as well, at least the value of the homogeneity scale has long been debated and most recently with quasars. The Universe has to be homogeneous and isotropic when it is viewed at suffjciently large scale. It requires/implies that the part of the Universe that we observe and study is a statjstjcally representatjve sample of its entjrety.

➢ Homogeneity = same observatjon can be made from wherever ➢ Isotropy = same observatjon can be made by looking in whatever directjon ➢ Isotropy for all observers implies homogeneity ➢ Homogeneity for all does not imply isotropy ➢ Bianchi cosmological models are homogeneous but anisotropic

Resurgent interests to explain some anomalies such as:

• Low-l defjcit in the TT angular power spectrum
• Small temperature variance
• Dipole and quadrupole alignment of moments
• Excess of Integrated Sachs-Wolfe efgect signal
• ...
• Departure from isotropic H0 from SNIa
• Extreme-scale alignments of quasar

(optjcal) polarizatjon vectors

• …

5

• V. Pelgrims

Cosmic Anisotropies from Quasars

from polarizatjon to structural-axis alignments

V.P. 2016, astro-ph: [arXiv:1604.05141]

Large-scale alignments of quasar polarizatjon vectors

 Cosmological principle: Isotropy and Homogeneity  Quasars: general propertjes and polarizatjon  Quasars and extreme-scale correlatjons  Quasars and large-scale structures

Quasars and Cosmology

6

• V. Pelgrims

Polarizatjon of light

Un-polarized Polarized

E B

7

• V. Pelgrims

Polarizatjon of light

E B

Un-polarized Polarized ψ = 30°

plin = 0 % plin >> 0 % N

8

• V. Pelgrims

Quasars: bright point-like sources in the Universe

~ 10’’

[Deep Field from Hubble Space Telescope]

9

• V. Pelgrims

Quasars: some propertjes

• Most luminous Actjve Galactjc Nuclei
• Ultra-bright point-like sources
• Emit light in the whole spectrum
• Observable at the far reaches of the

Universe

• Tiny region at the center of a Galaxy

(~ 10-3 – 10-4 pc) → matuer accretjon onto a Super Massive Black Hole (>108 Mʘ)

• Light is polarized at various

wavelengths → no spherical symmetry

[QSO 1229+204; Hutchings et al. 1994 (HST)]

~ 10’’

10

• V. Pelgrims

Quasars: some propertjes

• Most luminous Actjve Galactjc Nuclei
• Ultra-bright point-like sources
• Emit light in the whole spectrum
• Observable at the far reaches of the

Universe

• Tiny region at the center of a Galaxy

(~ 10-3 – 10-4 pc) → matuer accretjon onto a Super Massive Black Hole (>108 Mʘ)

• Light is polarized at various

wavelengths → no spherical symmetry

[Urry & Padovani; unified model]

11

• V. Pelgrims

Quasars: some propertjes

• Most luminous Actjve Galactjc Nuclei
• Ultra-bright point-like sources
• Emit light in the whole spectrum
• Observable at the far reaches of the

Universe

• Tiny region at the center of a Galaxy

(~ 10-3 – 10-4 pc) → matuer accretjon onto a Super Massive Black Hole (>108 Mʘ)

• Light is polarized at various

wavelengths → no spherical symmetry

• Very-high resolutjon observatjons of a

few showed the optjcal polarizatjon

• rientatjon relates to structural axis
• f the source (blue/UV contjnuum or

radio jet) [Borguet et al. 2005]

→ parallel or perpendicular to the spin axis at optjcal wavelength

~ 10’’

[Hutsemékers et al. 2015] [Smith et al. 2004]

12

• V. Pelgrims

Quasars: some propertjes

• Most luminous Actjve Galactjc Nuclei
• Ultra-bright point-like sources
• Emit light in the whole spectrum
• Observable at the far reaches of the

Universe

• Tiny region at the center of a Galaxy

(~ 10-3 – 10-4 pc) → matuer accretjon onto a Super Massive Black Hole (>108 Mʘ)

• Light is polarized at various

wavelengths → no spherical symmetry

• Very-high resolutjon observatjons of a

few showed the optjcal polarizatjon

• rientatjon relates to structural axis
• f the source (blue/UV contjnuum or

radio jet) [Borguet et al. 2005]

• Similar relatjon at other wavelength

[QSO 1229+204; Hutchings et al. 1994 (HST)]

~ 10’’

Quasars and extreme-scale correlatjons

Extreme-scale alignments of quasar optjcal polarizatjon vectors

13

• V. Pelgrims

Originally discovered: [Hutsemékers 1998] Confjrmed with:

• new observatjons

[Hutsemékers & Lamy 2001 ; Sluse et al. 2005]

• independent analyses

[Hutsemékers & Lamy 2001 ; Jain et al. 2004 ; Cabanac et al. 2005 ; Hutsemékers et al. 2005 ; Pelgrims & Cudell 2012 ; Pelgrims 2018]

A3

Probability of uniformity ~ 6 10-5

0.7 < z < 1.5

[Hutsemékers et al. 2005]

Right Ascension (°) Declinatjon (°)

Quasars and extreme-scale correlatjons

Extreme-scale alignments of quasar optjcal polarizatjon vectors

14

• V. Pelgrims

A3

Probability of uniformity ~ 6 10-5

0.7 < z < 1.5

[Hutsemékers et al. 2005]

Right Ascension (°) Declinatjon (°)

[Hutsemékers et al. 2005]

➢ Current sample:

355 quasars with reliable opt. pol.

➢ Signifjcant orientatjon correlatjons

within few Gpc scale regions

Quasars and extreme-scale correlatjons

Extreme-scale alignments of quasar optjcal polarizatjon vectors

15

• V. Pelgrims

A1 low z 0.0 < z < 1.0

[Hutsemékers et al. 2005]

Right Ascension (°) Declinatjon (°)

[Hutsemékers et al. 2005]

➢ Current sample:

355 quasars with reliable opt. pol.

➢ Signifjcant orientatjon correlatjons

within few Gpc scale regions

➢ Redshifu dependence of preferred

• rientatjon

Quasars and extreme-scale correlatjons

Extreme-scale alignments of quasar optjcal polarizatjon vectors

16

• V. Pelgrims

A1 1.0 < z < 2.3

[Hutsemékers et al. 2005]

Right Ascension (°) Declinatjon (°)

[Hutsemékers et al. 2005]

➢ Current sample:

355 quasars with reliable opt. pol.

➢ Signifjcant orientatjon correlatjons

within few Gpc scale regions

➢ Redshifu dependence of preferred

• rientatjon

Quasars and extreme-scale correlatjons

Extreme-scale alignments of quasar optjcal polarizatjon vectors

17

• V. Pelgrims

A1 1.0 < z < 2.3

[Hutsemékers et al. 2005]

Right Ascension (°) Declinatjon (°)

[Hutsemékers et al. 2005]

➢ Current sample:

355 quasars with reliable opt. pol.

➢ Signifjcant orientatjon correlatjons

within few Gpc scale regions

➢ Redshifu dependence of preferred

• rientatjon

➢ Statjstjcally signifjcant inside the whole

sample (including LEE) → probability of randomness <0.1% using dedicated statjstjcal tests

Quasars and extreme-scale correlatjons

Extreme-scale alignments of quasar optjcal polarizatjon vectors

18

• V. Pelgrims

[Hutsemékers et al. 2005]

➢ Current sample:

355 quasars with reliable opt. pol.

➢ Signifjcant orientatjon correlatjons

within few Gpc scale regions

➢ Redshifu dependence of preferred

• rientatjon

➢ Statjstjcally signifjcant inside the whole

sample (including LEE) → probability of randomness <0.1% using dedicated statjstjcal tests Stjll not understood today ! No satjsfactory explanatjon despite the various investjgated scenarios

• Cosmic strings/loops
• Cosmological-scale magnetjc fjeld
• Axion-like Dark Matuer partjcle
• Birefringence of the Universe
• Anisotropic cosmological expansion
• ...

[V.P. & Cudell 2014 ; V.P. 2014]

✔ Confjrmatjon of alignments with new and

statjstjcally independent methods

✔ Confjrmatjon of redshifu dependence but

with no smooth and contjnuous rotatjon as suggested before

[V.P. 2018]

✔ Robustness of alignments regarding

interstellar polarizatjon contaminatjon evaluated from Planck map

✔ But contaminatjon is detected for

~ 30% of the sample

Quasars and extreme-scale correlatjons

Extreme-scale alignments of quasar optjcal polarizatjon vectors

19

• V. Pelgrims

What can cause the polarizatjon alignments ?

➢ Photon path efgects

➢ Modulatjon of the

polarizatjon state

➢ Asymptotjc rotatjon of

the polarizatjon vectors

➢ Structural axis alignment

Quasars and extreme-scale correlatjons

Extreme-scale alignments of quasar optjcal polarizatjon vectors

20

• V. Pelgrims

What can cause the polarizatjon alignments ? Random Aligned

?

➢ Photon path efgects

➢ Modulatjon of the

polarizatjon state

➢ Asymptotjc rotatjon of

the polarizatjon vectors

➢ Structural axis alignment

Quasars and extreme-scale correlatjons

Extreme-scale alignments of quasar optjcal polarizatjon vectors

21

• V. Pelgrims

What can cause the polarizatjon alignments ?

➢ Photon path efgects

➢ Modulatjon of the

polarizatjon state

➢ Asymptotjc rotatjon of

the polarizatjon vectors

➢ Structural axis alignment

Aligned Aligned

?

Quasars and extreme-scale correlatjons

Extreme-scale alignments of quasar optjcal polarizatjon vectors

22

• V. Pelgrims

What can cause the polarizatjon alignments ?

➢ Photon path efgects

➢ Modulatjon of the

polarizatjon state

➢ Asymptotjc rotatjon of

the polarizatjon vectors

➢ Structural axis alignment

These scenario have difgerent observatjonal signatures Wavelength dependence of the alignments ?

Quasars and extreme-scale correlatjons

Quasar polarizatjon alignments in JVAS/CLASS 8.4 GHz surveys

23

• V. Pelgrims

Based on JVAS/CLASS 8.4-GHz surveys

[Jackson et al. 2007]

➢ Situatjon unclear from previous studies

[Joshi et al. 2007 ; Tiwari & Jain 2013 ; Shurtlefg 2014]

➢ Lack of consideratjon of the intrinsic

propertjes of the sources (redshifu, type, …) [V.P. & Hutsemékers 2015]

➢ Clear identjfjcatjon of 4155 Flat Spectrum

Radio Sources with reliable polarizatjon measurements (fpol > 1 mJy ; σψ ≤ 14° )

➢ Nasa Extragalactjc Database

→ redshifu for 1531 sources → Classifjcatjon in Object Types

[Pelgrims 2016]

QSO Radio Source Galaxies Various Object

with z informatjon no z

Group angular size (°)

[Pelgrims 2016]

Quasars and extreme-scale correlatjons

Quasar polarizatjon alignments in JVAS/CLASS 8.4 GHz surveys

[V.P. & Hutsemékers 2015]

➢ Evidence for alignment in one of the

region of optjcal pol. alignment (~3σ)

➢ Stat. signifjcant alignment features

within the whole sample

Dedicated global statjstjcal tests:

➢ comparison of polarizatjons in groups

• f nearest neighbors and averaged

with the whole sample

➢ 104 Monte Carlo simulatjons for

random distributjon

➢ For any given size of groups of

neighboring sources

→ 2D analysis with no restrictjon on the redshifu → For a wide range of size of groups of neighboring sources → For all subsamples at hand

p-value

24

• V. Pelgrims

Quasars and extreme-scale correlatjons

Quasar polarizatjon alignments in JVAS/CLASS 8.4 GHz surveys

[V.P. & Hutsemékers 2015]

➢ Evidence for alignment in one of the

region of optjcal pol. alignment (~3σ)

➢ Stat. signifjcant alignment features

within the whole sample Only for quasars!

➢ Identjfjcatjon of aligned groups

clustered towards regions where quasar polarizatjon vectors are aligned at optjcal wavelengths!

(A1 is roughly towards the same directjon of the alignment of the CMB di.quadru.octo pole moments)

[Pelgrims & Hutsemékers 2015]

A3 window A1 window

25

• V. Pelgrims

Radio wavelengths

➢ Photon path efgects

➢ Modulatjon of the

polarizatjon state

➢ Asymptotjc rotatjon of

the polarizatjon vectors

➢ Structural axis alignment

Quasars and extreme-scale correlatjons

Quasar polarizatjon alignments in JVAS/CLASS 8.4 GHz surveys

26

• V. Pelgrims

Radio wavelengths Optjcal wavelengths

➢ Photon path efgects

➢ Modulatjon of the

polarizatjon state

➢ Asymptotjc rotatjon of

the polarizatjon vectors

➢ Structural axis alignment ➢ Photon path efgects

➢ Modulatjon of the

polarizatjon state

➢ Asymptotjc rotatjon of

the polarizatjon vectors

➢ Structural axis alignment

?!?

Quasars and extreme-scale correlatjons

Quasar polarizatjon alignments: radio vs visible

27

• V. Pelgrims

28

• V. Pelgrims

Cosmic Anisotropies from Quasars

from polarizatjon to structural-axis alignments

V.P. 2016, astro-ph: [arXiv:1604.05141]

Large-scale alignments of quasar polarizatjon vectors

 Cosmological principle: Isotropy and Homogeneity  Quasars: general propertjes and polarizatjon  Quasars and extreme-scale correlatjons  Quasars and large-scale structures

Quasars and Cosmology

[SDSS Galaxies] a slice of our neighborhood

Quasars and large-scale structures

29

• V. Pelgrims

[Clowes et al. 2013] → discovery of a big inhomogeneity in the quasar distributjon

the Huge-LQG, next to the CCLQG Huge-LQG

➢ z ~ 1.3 ➢ 73 quasars ➢ elongatjon ~ 1 Gpc !

[Clowes et al. 2013]

Declinatjon (°) Right Ascension (°) 30

• V. Pelgrims

Quasars and large-scale structures

much bigger than the homogeneity scale of the Universe … A problem that has fjnally been solved:

[see: Nadathur 2013 ; Einasto et al. 2014 ; Parkes et al. 2015 and fjnally [Marinello et

• al. 2016]

[Clowes et al. 2013] → discovery of a big inhomogeneity in the quasar distributjon

the Huge-LQG, next to the CCLQG

The Huge-LQG (and the CCLQG) is at the outskirt (3D) of one of the regions of optjcal polarizatjon alignments of quasars

[Clowes et al. 2013] [Pelgrims 2016]

Declinatjon (°) Right Ascension (°) Right Ascension (°) Right Ascension (°) 31

• V. Pelgrims

Quasars and large-scale structures

[Hutsemékers, Braibant, V.P., Sluse 2014]

➢ Polarizatjon in the Huge-LQG and CCLQG

[Hutsemékers et al. 2014]

Declinatjon (°) Right Ascension (°) 32

• V. Pelgrims

Quasars and large-scale structures

[Hutsemékers et al. 2014]

Declinatjon (°) Right Ascension (°) Relatjve Angle (°)

Quasar spin-axes align with the large-scale structures at z ~ 1.3 and over cosmological scales !

33

• V. Pelgrims

[Hutsemékers, Braibant, V.P., Sluse 2014]

➢ Polarizatjon in the Huge-LQG and CCLQG

Quasars and large-scale structures

~ 1 Gpc

Quasar spin-axes preferentjally parallel to the major axes of rich large quasar groups at high redshifus and over large scales !

Relatjve Angle (°) 34

• V. Pelgrims

Quasars and large-scale structures

[V.P. & Hutsemékers 2016]

➢ Radio polarizatjon in a large LQG sample ➢ Polarizatjon (synchrotron) is preferentjally ┴ to quasar spin axis [Joshi et al. 2007]

1.0 < z < 1.8

Explained through coevolutjon of galaxy spin axes within the cosmic web ?

Involved scales seem too large ...

35

• V. Pelgrims

Quasars and large-scale structures

Corroborated by

➢ degree scale radio-jet axis correlatjons

• [Taylor & Jagannathan 2016]

→ alignments in 1.4 deg2 ELAIS N1 fjeld

• [Contjgiani et al. 2017]

→ alignments at scale 1.5–2.5 deg in 7000 deg2 FIRST+RadioGalaxyZoo sample (30 059 sources)

➢ degree scale radio-polarizatjon correlatjons

• [V.P. & Hutsemékers 2015]

→ alignments < 5 deg found in JVAS/CLASS 8.4GHz

[Taylor & Jagannathan 2016]

[Hutsemékers, Braibant, V.P., Sluse 2014 ; V.P. & Hutsemékers 2016]

➢ Made use of optjcal and radio polarizatjon of quasars

to infer their spin axes at high redshifu

➢ Show quasar spin-axes correlate to the major axes of

their host LQG

There are evidences for extreme-scale alignments of the polarizatjon

• f quasars when measured at optjcal and at radio wavelengths

➢ Origin is stjll to be found ➢ Could indicate departure from isotropy of the Universe given the

characteristjc size of the correlatjon

➢ Difgerence between optjcal and radio signatures needs to be clarifjed

The large-scale correlatjon of quasar spin axes with and within large quasar groups

➢ Could be due to coevolutjon of black hole spins in LSS ➢ Typical size involved are way larger than expected

→ large-scale intrinsic alignments of galaxies ???

If true… the two types of alignments could fjnd the same origin assuming anisotropy in large-scale structure orientatjons

36

• V. Pelgrims

Take away

Quasar polarizatjon alignments

[Artjst view of the “spooky” alignment Credit: ESO/M. Kornmesser]

37

• V. Pelgrims

Thank you

BACKUP