THE COMPLEX GAS KINEMATICS IN THE NUCLEAR REGION OF NGC 7213
PhD student: Francesco Salvestrini Supervisor: Cristian Vignali Co-supervisors: Carlotta Gruppioni Francesca Pozzi Collaborator: Rosita Paladino Different gas components
Optical/Uv emission Warm dust emission Cold molecular from the accretion disc Coronal X-ray from the torus (few pc) gas and dust (several Rg scales) emission
Molecular cloud
Spiral arm Different gas components
Coronal X-ray emission
Iron Kα line
LX LAGN -� E × F(E) [arbitrary N~ N0 × e reflection hump � ~ x σT NH
Courtesy of R. E Different gas components
Warm dust emission Cold molecular from the torus (few pc) gas and dust
SFR
Ldust Mdust Different gas components
Molecular gas kinematic CO SLED Molecular PDR+XDR fiducial model gas ] -2 cm -1 erg s erg -15 CO flux [10
Salvestrini et al. in prep. (paper I) Mingozzi et al. 2017 Jup
ΣH2 = αCO ICO NGC 7213
Local S0 galaxy (z=0.005839, 1”~120pc) spectroscopically classified as Seyfert (Phillips 1979) / LINER (Filippenko & Halpern 1984). Available data: ‣ X-ray: NuSTAR + XMM-Newton (+ Suzaku + Chandra) ‣ optical: SALT spectrum ‣ mid-IR: IRS spectrum ‣ sub-mm: ALMA Band 6 CO(2-1) ‣ sub-mm: APEX PI230 (?) ‣ radio: 4.8, 8.4, 20 GHz NGC 7213
Local S0 galaxy (z=0.0058, 1”~120pc) spectroscopically classified as Seyfert (Phillips 1979) / LINER (Filippenko & Halpern 1984) Available data: ‣ X-ray: NuSTAR + XMM-Newton (+ Suzaku + Chandra) optical: SALT spectrum Nustar (3-79 keV) ‣ ‣Exp. time: 101.6 ks ‣Angular res.: 16" (FWHM) ‣ mid-IR: IRS spectrum ‣Energy res.: 400 eV at 6 keV XMM-Newton (3-10 keV) ‣ sub-mm: ALMA Band 6 CO(2-1) ‣Exp. time: 132.5 ks Angular res.: 6” (FWHM, on-axis) radio: 4.8, 8.4, 20 GHz ‣ ‣ ‣Energy res.: 150 eV at 6 keV L2-10keV ~ 1042 erg s-1 F2-10keV ~ 10-11 erg s-1 cm-2
NH ~ 1022 cm-2 �~1.9
-FPMA -FPMB } Nustar -PN -MOS1 XMM-Newton -MOS2 } NGC 7213
Local S0 galaxy (z=0.005839, 1”~120pc) spectroscopically classified as Seyfert (Phillips 1979) / LINER (Filippenko & Halpern 1984) Available data: ‣ X-ray: NuSTAR + XMM-Newton (+ Suzaku + Chandra) ‣ optical: SALT spectrum ‣ Project_code: 2012.1.00474.S ‣ mid-IR: IRS spectrum ‣ PI_name: Nagar, N. ‣ Band: 6 ‣sub-mm: ALMA Band 6 CO(2-1) ‣ Spatial res.: 0.52” ‣ LAS: 6.3” ‣ radio: 4.8, 8.4, 20 GHz ‣ Spectral res.: 10 km/s CO (2-1) emission line map 48” 229.2 GHz 51”
54”
57”
-47°10’00”
03”
”
J2000 Declination 06
09”
12” ~60 pc
22h09m17s.5 16s.5 16s.0 15s.5 15s.0 J2000 Right Ascension CO (2-1) emission line map 48” 229.20859018 GHz 51”
54”
57” Region A
-47°10’00” ~ 180pc x 300 pc 03” Region A ”
J2000 Declination 06
09”
12” ~60 pc [mJy/beam] 22h09m17s.5 16s.5 16s.0 15s.5 15s.0 J2000 Right AscensionVelocity [km/s] CO (2-1) emission line map 48” 229.2 GHz 51”
54”
57” Region B
-47°10’00” R~0.5” ~3.3” (400 pc) NE from the nucleus 03”
”
J2000 Declination 06
09”
12” ~60 pc
22h09m17s.5 16s.5 16s.0 15s.5 15s.0 J2000 Right Ascension CO (2-1) emission line map 48” 229.2 GHz 51”
54”
57” Region C -47°10’00” ~ 150pc SE from the nucleus
03” Region C See PV diagram later! ”
J2000 Declination 06
09”
12” ~60 pc [mJy/beam]
22h09m17s.5 16s.5 16s.0 15s.5 15s.0
J2000 RightVelocity Ascension [km/s] Major axis PV diagram
Di Teodoro & Fraternali 2015
8 rings (1.5”, ~180pc)
Major axis Minor axis PV diagram
Minor axis REGION C
Salvestrini et al. in prep. (paper I) DATA MODEL
Minor axis INTENSITY
Intensity [Jy km/s]
Salvestrini et al. in prep. (paper I) DATA MODEL
Minor axis VELOCITY
VLOS [km/s]
Salvestrini et al. in prep. (paper I) DATA MODEL
Minor axis DISPERSION
σ [km/s]
Salvestrini et al. in prep. (paper I) 57” ALMA Band 6 continuum: 120 pc point-like source 58”
59”
-47°10’00”
01” J2000 Declination
02”
03” 22h09m16s.5 16s.3 16s.2 16s.1 16s.0 J2000 Right Ascension ALMA Band 6 continuum: 120 pc point-like source
Synchrotron radiation? -47°10’00”
01” dust J2000 Declination re-emission 02”
03” stars 22h09m16s.5 16s.3 16s.2 16s.1 16s.0 J2000 Right Ascension torus
synchrotron ALMA continuum
Fig. 3Gruppioni et al. 2016 -Optical peak emission -ALMA continuum 1 kpc -CO(2-1) emission Conclusions ‣ Relatively weak AGN not affecting the ISM. ‣ Kinematical modelling of the molecular gas component. ‣ Potential outflow? … and more to do! ‣ Mdust from detected continuum ‣ Mgas from APEX PI230 (?) ‣ New optical classification on proprietary SALT data
More details in Salvestrini et al. in prep. Thank you! BACKUP SLIDES The sample The sample
‣ 12MGS is a mid-IR selected sample ( F12μm > 0.22 Jy ) consisting of 893 galaxies. 118 classified as AGN ‣ Our sample consists of 76 galaxies having mid-IR spectra (5.5–35 μm & 10-37 μm). ‣ 26/76 galaxies having far-IR Herschel-PACS (~60-200 μm) and -SPIRE (~200-600 μm) spectra. ‣ Galaxies are classified as Seyfert 1, 2 (35/76, 38/76) and LINER (3/76). ‣ 0.0023 < z < 0.1849 The sample
‣ 12MGS benefits from an extensive data set, from X-ray to radio frequencies from different observational campaigns spread over the past 20 years.
-dust re-emission The SED decomposition has -unobserbed stars ‣ -estinguished stars been performed over the -torus entire sample of 76 galaxies (Gruppioni et al. 2016).
•LAGN •SFR •�(AGN) •M★
Gruppioni et al. 2016 Herschel SPIRE & PACS spectrographs
NH from the 9.7μm feature
- stars - torus 0.042 - dust
21 −2 NH ∼ 2 · 10 τVlos cm Compton depth
Compton depth is defined as the Thomson depth of the medium regard- less of the energy spectrum of the incident photons
• X-ray source is isotropic • Column-density distribution is spherically-symmetric
NGC 7213 Region B
R~0.5” ~3.3” (400 pc) NE from the nucleus
Region A
0.5
-0.5 [mJy/beam]
Velocity [km/s] CO (2-1) emission line map 48” 229.20859018 GHz 51”
54”
57” Region A
-47°10’00” ~ 180pc x 300 pc 03” Region A ”
J2000 Declination 06
09”
12” ~60 pc [mJy/beam] 22h09m17s.5 16s.5 16s.0 15s.5 15s.0 J2000 Right AscensionVelocity [km/s] Spettro IR NGC7213
NGC 7213 z=0.005839
Gruppioni et al. 2016 L2-10keV = (9+100-2)×1041 erg s-1
F2-10keV = (1.1+13-0.9)×10-11 erg s-1 cm-2
NH = (1.63+0.17-0.14)1022 cm-2 �=1.8+0.3-0.1
-FPMA -FPMB } Nustar -PN -MOS1 XMM-Newton -MOS2 } Quasar as High-Redshift Standard Candles
The LX-LUV relation at high redshift
Co-authors: G. Risaliti, S. Bisogni, E. Lusso
Salvestrini et al. (in prep.) The LX-LUV relation
Avni and Tananbaum (1986)
Lusso et al. (2010) �intr ~ 0.35-0.40 dex The LX-LUV relation
‣ SDSS DR7 (Shen et al. 2011) ‣ 3XMM-DR5 ‣ No BAL sources ‣ Radio Quiet
1.6 < X < 2.8 0.6 0.65 ‣ � ⇠ ‣ 2153 sources ‣ 0.065 < z < 4.925
Lusso and Risaliti (2016) The sample
‣ SDSS DR7 (Shen et al. 2011) & DR12 (for z<5.3) Accurate selection ‣ No BAL sources ‣ Radio Quiet } ‣ Archival Chandra and Accurate X-ray XMM-Newton observations analysis ‣ No X-ray flux upper limit ‣ 4.0 < z <7.08 Evolution with redshift?
More details in: Salvestrini et al. in prep. +0.12 =0.51 0.12 =0.22 dex