QSO project: Giant Lyman alpha nebula around the hyper-luminous quasar SDSS J1538+0855

(1)

2018 Publication Year

2020-10-19T09:51:09Z Acceptance in OA@INAF

Title

TRAVASCIO, ANDREA; PICONCELLI, Enrico; ZAPPACOSTA, Luca; Cantalupo, S.; FIORE, Fabrizio; et al.

Authors 10.5281/zenodo.1471643 DOI http://hdl.handle.net/20.500.12386/27882 Handle 13 Number

(2)

QSO project:

Giant Lyα Nebula around the hyper-luminous

quasar SDSS-J1538+0855

Andrea Travascio (INAF OAR, Sapienza, Tor Vergata)

Collaborators OAR and more

**E. Piconcelli, L. Zappacosta, S. Cantalupo*, F. Fiore,

M. Ginolfi, A. Bongiorno, M. Bischetti, G. Vietri, F. Duras, A. Luminari

(3)

CGM QSO Outflows ISM

Circum-Galactic Medium (CGM)

• Circum-Galactic Medium

(CGM) is the gas surrounding

galaxies outside their disks

(>15 kpc) and inside their

virial radii.

• Observations and simulations

indicate that the CGM is

‣

the venue for galactivc

feedback and recycling

‣

the reserve of galaxies

star-forming fuel (Evidences of

CGM in inflow?)

CGM has a key role in galaxy evolution and in the

AGN feeding & feedback cycle

‣

the key regulator of the galactic gas supply

(4)

‣ Mechanisms of emission:

- collisional excitation (Haiman+00)

- resonant scattering from the quasar BLR

(Cantalupo+05)

- fluorescent (photoionization+recombination)

(Hogan & Weymann 1987, Cantalupo+12)

‣ Lyα line: λ=1215.67 A

‣ hν=10.2 eV, t=1.59 ns

‣ Resonant scattering

‣ Random walk in frequency and position: escaping from the system

RVIR UV source γ_Lyα HI clouds HII Photo-ionization & Recombination T~ 104_K

Lyα emission

simulation analytic solution

probabilit y distribution of escaping photons

Cantalupo+05 τ(λ) = ( N_HI 1017.2_cm−2₎₍ λ 912Å ) 3

(5)

Giant Lyα Nebulae in the past

Cantalupo+14 (Nature) 460 k pc Van Ojik+96 1242+036

‣ Giant Lya nebulae around High z Radio Galaxies

(HzRGs) (Lilly & Longair 84, Van Ojik+96, Adam+97)

‣ L~1045_{erg/s, size up to ~200 kpc}

‣ Optical/UV and radio emissions spatially correlated (McCarthy+87)

‣ photoionization + shock-ionization (Villar Martin+97)

‣Discovered in Narrow Band (NB) imaging a Enormous Lyman-Alpha Nebulae (ELAN)

around multiple radio quiet QSOs (RQQs) z~2.3

‣do not have radio-jets that may power Lya emission on large scales

‣size 460 kpc (beyond the virial radius) and L~2 x 1044_erg/s

(6)

MUSE

integral-field spectrograph

Giant Lyα Nebulae with MUSE (GLAN)

‣ MUSE Optical integral-field spectrograph -No filter and slit losses

‣ FoV 1’x1’, pixel scale 0.2 “/pixel

-at redshift z=3.5: FoV (450x450 kpc2_{), pixel}

scale (1.5 kpc/pixel) -High sensitivity

★

Advent of Multi Unit Spectroscopic Explorer (MUSE)

‣GLAN are ubiquitous (detection rate 100%)

around RQQs at z~3-4 within at least 50 kpc (Borisova+16)

‣see also Ginolfi+18, Arrigoni-Battaia+18

(7)

‣ Sample of ~86 broad-line WISE/SDSS Selected

Hyper-luminous (WISSH) quasars

‣ Bolometric Luminosity log(Lbol) > 47.2, z>1.5 and WISE(22$m) > 3 mJy

‣ Aims: AGN feedback in the most luminous

quasars of the Universe

the WISSH QSO project: MUSE

★

WISSH MUSE PROJECT

‣ Studying the CGM around the most luminous quasars of the Universe with powerful outflows

‣ probe presence of possible AGN driven winds bejond host galaxy

‣ shedding light on AGN feeding and feedback

★_Aims:

Bischetti+17,+18, Martocchia+17, Duras+17, Vietri+18, Bruni+ in prep

‣ 7 WISSH QSOs targeted by MUSE

‣ 2 are proprietary data (PI Fiore) (J1538+08, J2238-08)

(8)

3 2 2.1 7.4 13 18 24 29 34 40 45 50 31.2 30.8 30.4 15:38:30.0 25.0 8:55:20.0 15.0 10.0 5 .0 3 2 2.1 7.4 13 18 24 29 34 40 45 50 31.2 30.8 30.4 15:38:30.0 25.0 8:55:20.0 15.0 10.0 5 .0 SB Ly α (10 −18 erg s −1 cm −2 arc sec −2 )

PSF

30 kpc

Giant Lyα nebula around J1538

‣ Obtained with

CubExtractor, a tool to perform PSF-subtraction and low surface brightness detection/analysis (Cantalupo+in prep) ‣ Maximum size 144 kpc ‣ Integrated SNR(Lyα)~30 ‣ zQSO=3.567, zLyα= 3.563 ‣ LLyα=2.04 x 1044 erg/s SNR >2.5 propagated SNR levels

•

QSO (1 x 1 arcsec2₎

★

_{SB peak in the south region of the nebula (UV radiation cone)}

(9)

SB Ly α (10 −18 erg s −1 cm −2 arc sec −2 )

PSF

0 064 0.94 1.9 3 4 5 6 7 8 9 10 31.2 30.8 30.4 15:38:30.0 25.0 8:55:20.0 15.0 10.0 5 .0 0 064 0.94 1.9 3 4 5 6 7 8 9 10 31.2 30.8 30.4 15:38:30.0 25.0 8:55:20.0 15.0 10.0 5 .0 30 kpc

Surprise: discovery of giant CIV nebula

3 2 2.1 7.4 13 18 24 29 34 40 45 50 31.2 30.8 30.4 15:38:30.0 25.0 8:55:20.0 15.0 10.0 5 .0 3 2 2.1 7.4 13 18 24 29 34 40 45 50 31.2 30.8 30.4 15:38:30.0 25.0 8:55:20.0 15.0 10.0 5 .0 SB Ly α (10 − 18 er g s ₋ 1 cm − 2 ar cs ec ₋ 2 ) PSF 30 kpc ‣ Maximum size 60 kpc ‣ Integrated SNR(Lyα)~5 ‣ zQSO=3.567, zCIV= 3.562 ‣ LCIV=9.63 x 1042 erg/s

★

_{Discovery a CIV nebula in the same south region}

★

_{CGM metal-rich}

★

_{Which mechanism has transported the CIV up to here?}

‣

Outflow? Stellar feedback?

PSF

(10)

F

No rm Nebula Lyα quasar Lyα velocity [× 1000 km/s] blue tails

★

_{Blue tail of the Lyα emission line in the}

nebula spectrum: could it suggests the

presence of an outflow? (Verhamme+14)

Lyα line profile: blue tail = outflow?

Nebula CIV velocity [× 1000 km /s]

F

No rm quasar CIV Verhamme+14

‣

Is it a simple Lyα blue component?

‣

Is it the second peak that we would

observe typical for a resonant line?

★

_{What is the spatial distribution of this}

(11)

blue tail spatially resolved

‣

Skewness map

‣

It gives an indication of the

Lyα emission line asymmetry

and its spatial distribution

★

_{The Ly a profile is more skewed towards negative values in the SB peak}

of the nebula. Why?

‣

Can we just resolve the blue tail with an higher SNR?

‣

Is it indicating the presence of an outflow?

0 00059 -0.00049 -0.00039 -0.00029 -0.00019 -9.4e-05 5.3e-06 0.0001 0.0002 0.0003 0.0004 0 00059 -0.00049 -0.00039 -0.00029 -0.00019 -9.4e-05 5.3e-06 0.0001 0.0002 0.0003 0.0004

I

3

=

μ

3

_/μ

3/22 PSF

‣

pixel value distribution

• Work in progress! Any comments or suggestions please? :)

positive values

negative values

(12)

blue tail spatially resolved

‣

Skewness map

‣

It gives an indication of the

Lyα emission line asymmetry

and its spatial distribution

★

_{The Ly a profile is more skewed towards negative values in the SB peak}

of the nebula. Why?

‣

Can we just resolve the blue tail with an higher SNR?

‣

Is it indicating the presence of an outflow?

0 00059 -0.00049 -0.00039 -0.00029 -0.00019 -9.4e-05 5.3e-06 0.0001 0.0002 0.0003 0.0004 0 00059 -0.00049 -0.00039 -0.00029 -0.00019 -9.4e-05 5.3e-06 0.0001 0.0002 0.0003 0.0004

I

3

=

μ

3

_/μ

3/22 PSF

‣

pixel value distribution

• Work in progress! Any comments or suggestions please? :)

positive values

negative values

(13)

1407 -1218 -1029 -839 -650 -459 -270 -81 109 298 487 1407 -1218 -1029 -839 -650 -459 -270 -81 109 298 487 Ve loc ity [k m /s]

30 kpc

6 9e+02 -5.9e+02 -4.9e+02 -4e+02 -3e+02 -2e+02 -1e+02 -8 90 1.9e+02 2.8e+02 6 9e+02 -5.9e+02 -4.9e+02 -4e+02 -3e+02 -2e+02 -1e+02 -8 90 1.9e+02 2.8e+02 Ve loc ity [km /s]

30 kpc

PSF PSF

Velocity map with respect to the z

QSO

★ _{blue-shifted bulk motion of the Lya Nebula relative to the systemic z as}

determined from the Hβ —> hint of an outflow?

✓ _{We need to have molecular lines from the host galaxy in order to a reliable}

systemic redshift of the QSO and constrain the nebula kinematic

✓ _{We need to have non-resonant line (Hα, HeII etc…)}

‣problem to find the systemic redshift of the QSO

‣complex radiative transfer effects = complex kinematic interpretation

(14)

300 370 440 510 580 650 720 790 860 930 1000 300 370 440 510 580 650 720 790 860 930 1000

30 kpc

PSF Ve loc ity dis pe rsi on [km /s] 1 7e+02 2.3e+02 3e+02 3.6e+02 4.2e+02 4.9e+02 5.5e+02 6.1e+02 6.7e+02 7.4e+02 8e+02 1 7e+02 2.3e+02 3e+02 3.6e+02 4.2e+02 4.9e+02 5.5e+02 6.1e+02 6.7e+02 7.4e+02 8e+02

QSO project: Giant Lyman alpha nebula around the hyper-luminous quasar SDSS J1538+0855

QSO project:

Giant Lyα Nebula around the hyper-luminous

quasar SDSS-J1538+0855

Andrea Travascio (INAF OAR, Sapienza, Tor Vergata)

Collaborators OAR and more

E. Piconcelli, L. Zappacosta, S. Cantalupo*, F. Fiore**,

M. Ginolfi, A. Bongiorno, M. Bischetti, G. Vietri, F. Duras, A. Luminari

Circum-Galactic Medium (CGM)

•

Circum-Galactic Medium

(CGM) is the gas surrounding

galaxies outside their disks

(>15 kpc) and inside their

virial radii.

•

Observations and simulations

indicate that the CGM is

the venue for galactivc

feedback and recycling

the reserve of galaxies

star-forming fuel (Evidences of

CGM in inflow?)

CGM has a key role in galaxy evolution and in the

AGN feeding & feedback cycle

the key regulator of the galactic gas supply

Lyα emission

Giant Lyα Nebulae in the past

Giant Lyα Nebulae with MUSE (GLAN)

Advent of Multi Unit Spectroscopic Explorer (MUSE)

the WISSH QSO project: MUSE

WISSH MUSE PROJECT

PSF

Giant Lyα nebula around J1538

•

★

SB peak in the south region of the nebula (UV radiation cone)

PSF

Surprise: discovery of giant CIV nebula

★

Discovery a CIV nebula in the same south region

★

CGM metal-rich

★

Which mechanism has transported the CIV up to here?

‣

Outflow? Stellar feedback?

F

★

Blue tail of the Lyα emission line in the

nebula spectrum: could it suggests the

presence of an outflow? (Verhamme+14)

Lyα line profile: blue tail = outflow?

F

‣

Is it a simple Lyα blue component?

‣

Is it the second peak that we would

observe typical for a resonant line?

★

What is the spatial distribution of this

blue tail spatially resolved

‣

Skewness map

‣

It gives an indication of the

Lyα emission line asymmetry

and its spatial distribution

★

The Ly a profile is more skewed towards negative values in the SB peak

of the nebula. Why?

‣

Can we just resolve the blue tail with an higher SNR?

‣

Is it indicating the presence of an outflow?

I

=

μ

/μ

‣

**E. Piconcelli, L. Zappacosta, S. Cantalupo*, F. Fiore,

_{SB peak in the south region of the nebula (UV radiation cone)}

_{Discovery a CIV nebula in the same south region}

_{CGM metal-rich}

_{Which mechanism has transported the CIV up to here?}

_{Blue tail of the Lyα emission line in the}

_{What is the spatial distribution of this}

_{The Ly a profile is more skewed towards negative values in the SB peak}

_/μ

_{The Ly a profile is more skewed towards negative values in the SB peak}

_/μ

_{high turbolence in the central region of the nebula}

_{∼ 1300 km/s}

_{∼ 700 km/s}

_{Lyα nebula has size ~ 144 kpc with L}

_{~ 10}

_erg/s

_{CIV nebula shows size ~60 kpc with L}

_{~ 10}

_erg/s

_{The line profiles and the velocity maps suggest that we are}

_{estimate the systemic redshift of the quasar through a line that}

_{look for a non resonant emission line (e.g. Hα, HeII..)}

_{Powerful outflows are a plausible mechanism capable of bringing}