Optical spectroscopy of nearby type-1 LINERs Cazzoli et al. 2018 Optical Spectroscopy of local type-1 AGN LINERs S. Cazzoli et al. 2018 MNRAS, 480, 1106-11162 I. Marquez , J. Masegosa , A. del Olmo, M. Povic , O. Gonzalez- Martin , B. Balmaverde , L. Hernandez-Garcia , S. Garcia-Burillo
Optical spectroscopy of nearby type-1 LINERs Cazzoli et al. 2018 L ow I onisation N uclear E mission-line R egion s LINERs are LLAGNs L H α ∼ 0.5-3.7 × 10 39 erg/s L X [2 − 10 KeV ] ∼ 1.2-8.8 × 10 39 erg/s and Ho+08 Heckman+80 Filipenko+92 Dopita+96 Shields+97 Intensity [A.U.] Ho+97,+03, +08 Elitzur&Shlosman+06 Gonzalez-Martin+09 Singh+13 Elitzur+2014 Balmaverde+14,+16 Netzer+2015 Constantin+15 Padovani+17 Marquez+2017 ... Wavelength [A] N arrow L ines B road L ines Strong low-ionisation and faint Faint high-ionisation emission lines Does the BLR disappear? Different profiles, stratification of the NLR?
Optical spectroscopy of nearby type-1 LINERs Cazzoli et al. 2018 Optical emission: BPTs diagnostic diagrams Baldwin+81 Diagnostic diagrams: BPTs (Baldwin+1981) The ionisation mechanism of optical lines is debated: AGNs – e.g. Heckman+80 Shock-heating models – e.g. Kewley+01 pAGBs stars models – e.g. Sarzi+10, Singh+13 Which is the dominant ionisation mechanism?
Optical spectroscopy of nearby type-1 LINERs Cazzoli et al. 2018 Galaxy evolution and outflows LINERs are important population to study: Ho+08 Most numerous local AGN population Bridge the gap between normal and luminous active galaxies LINERs are unexplored laboratory for outflows !! Very few works, mainly via H α imaging, e.g. Pogge+00, Masegosa+11 Detection rate? kinematics ? Does the broadening of lines hamper the detectability of the BLR component? Veilleux+05, review NGC4438 arcsec M 82 M 82 optical+IR H α Hubble archive arcsec Masegosa+11 OUTFLOW NGC1052 - Cazzoli+18 H α -[NII] [SII] [OIII] [OI] H β Smith, Gallagher & Westmoquette
Optical spectroscopy of nearby type-1 LINERs Cazzoli et al. 2018 Optical spectroscopy of nearby type-1 LINERs, Cazzoli+18 LINER-population as a case of study: Does the BLR disappear ? Is the NLR stratified ? Which is the dominant ionisation mechanism? Are outflows frequent ? Most numerous local AGN population Bridge the gap between normal and luminous active galaxies Our Goals: Detectability and properties of the BLR component Low and high ionisation lines do (not) have the same profiles Discriminate between ionisation: from AGN, shocks and pAGBs Frequency and kinematics of outflows Type 1 LINERs, L1 = ⇒ direct sight, BLR visible
Optical spectroscopy of nearby type-1 LINERs Cazzoli et al. 2018 Sample: 22 L1 from the Palomar Survey, Ho+97 All L1 in the Northern hemisphere, z ∼ 0.006, D ∼ 30Mpc (on average) • Genuine AGNs from X-rays studies (Gonz´ alez-Mart´ ın+09, Hern´ andez-Garc´ ıa+14) Ground-based spectra from H β to [SII] TWIN @ CAHA 3.5m 20 LINERs slit width 1.2” – 0.5 ˚ A/pixel ALFOSC @ NOT 2.5m 2 LINERs slit width 1.0” – 1.5 ˚ A/pixel NGC4203 excluded Space-based spectra from [OI] to [SII] double peaked H α from the accretion disc HST / STIS (Balmaverde+14) 12 LINERs ground: 21 L1 space: 11 L1 slit width ≤ 0.2” – 0.6 ˚ A/pixel
Optical spectroscopy of nearby type-1 LINERs Cazzoli et al. 2018 Strategy STELLAR MODELING and SUBTRACTION : 3 techniques pPXF (Cappellari+17), STARLIGHT (Cid Fernandez+11), ‘template galaxies’ (Ho+08) MODELS : [OI] and/or [SII] as template for the H α -[NII] blend n [SII] [OI] H α - [NII] o ] I i I t S a [ c ) i 1 f i t a r t s o n [OI] [SII] H α - [NII] n o H α ] I i O t a [ c ) i 2 f i BROAD t a r t s o [SII] [NII] [OI] H α n ] I O n o [ d i t n a a c i ] f I i [SII] [OI] H α - [NII] I t S a [ r t ) 3 s R L N THREE COMPONENTS FOR EMISSION LINES (ionised gas) : Narrow, Second and Broad (AGN) TWO COMPONENTS FOR ABSORPTION NaD LINES (neutral gas)
Optical spectroscopy of nearby type-1 LINERs Cazzoli et al. 2018 On the AGN nature of LINERs NLR stratification is often present in L1 Ground: 9/21 vs. Space: 5/11 The broad H α component is ubiquitous in HST spectra ONLY Ground: 7/21 vs. Space: 11/11 Difference of > 1000 km/s with previous measurements the FWHM(H α ) Choice of the model, number of components and stellar subtraction ♣ .. what about type-2? Hermosa-Mu˜ noz+19 POSTER ground: CAHA/TWIN space: HST/STIS NGC4450 NGC4450 NARROW [OI] NARROW [OI] 2.0 4000 H α -[NII] 1.5 H α -[NII] BROAD [SII] BROAD [SII] Flux [erg/cm /s/Å] [SII] Flux [erg/cm /s/Å] 3000 Flux [AU] [SII] [OI] 1.0 [OI] 2000 BROAD [OI] BROAD [OI] 0.5 1000 0.0 VERY BROAD H 0.10 600 Residuals Residuals 6300 6400 6500 6600 6700 6300 6400 6500 6600 6700 Wavelength Wavelength
Optical spectroscopy of nearby type-1 LINERs Cazzoli et al. 2018 Non rotational motions and kinematic classification Second component, possibly associated to non rotational motions, seem common Ground: 14/21 vs. Space: 7/11 Kinematic classification: the σ -V diagram Limits from rotation curves Narrow component: rotation – all cases Second component: all possibilities, outflow detection rate ∼ 60 % s Narrow Second s 600 e e Rotation s Candidates t Rotation a e t Rotation Rotation a t Narrow Component Second Component d a Component Component d d i d i i d d n 400 n n a a a C C C Velocity [km/s] 200 − − Inflows Inflows Inflows Inflows 0 Ouflows Ouflows Ouflows Ouflows − − 200 − − 400 − − 600 0 200 400 600 800 1000 1000 0 0 200 400 600 800 1000 σ [km/s] σ [km/s] Velocity dispersion [kms − − 1 ] Velocity dispersion [kms − 1 ] − ground space
Optical spectroscopy of nearby type-1 LINERs Cazzoli et al. 2018 Discriminating ionisation mechanisms: narrow component BPTs constraints Dividing curve by Kauffmann+03, Kewley+06, Filipenko+92 AGN (Allen+08) and pAGBs (Binette+04) models N el : 100 cm -3 Log U : Models: AGNs Weak [OI] Strong [OI] > 0.16 -3.6 -3.0 0.0 pAGBs 2.0 Sy Sy Sy Narrow Component Sy Sy Sy 1.5 LOG [O III] / H β LOG ([OIII] / H β ) 1.0 0.5 0.0 LINER LINER LINER LINER LINER LINER HII - SF − 0.5 HII - SF HII - SF HII − SF HII − SF HII − SF − 1.0 -1.0 -0.5 0.0 0.5 -1.5 -1.0 -0.5 0.0 0.5 -2.0 -1.5 -1.0 -0.5 0.0 0.5 LOG [N II] / H α LOG [S II] / H α LOG [OI] / H α AGN as the dominant mechanism of ionisation
Optical spectroscopy of nearby type-1 LINERs Cazzoli et al. 2018 Discriminating ionisation mechanisms: second component As for the narrow component but we focus [OI] BPT: the most sensitive to shocks Shocks models reproduce well the line ratios for the second component [OI] BPT + shocks models (Groves+04) + kinematic measurements/classification 2.0 2.0 shock velocity s Sy Sy w Sy Second Component n Sy Sy Sy o o 1.5 1.5 i l f LOG [O III] / H β t a t u t β β β o O β 1.0 1.0 R C s w o 0.5 0.5 l f n I 0.0 0.0 ER LINER LINER LINER LINER LINER LINER LINER − 0.5 H − − − 0.5 HII - SF − HII - SF − − H HII - SF − − HII − SF − HII − SF − HII − SF − − − 1.0 − − − 1.0 − 1.5 − − − − − − − − − − 0.5 -2.0 -1.5 -1.0 -0.5 0.0 0.5 -2.0 -1.5 -1.0 -0.5 0.0 0.5 0.5 -2.0 -1.5 -1.0 -0.5 0.0 0.5 − − − − − − − − − − − − − − − − − 2.5 − 2.0 − 1.5 − 1.0 − 0.5 − − − − − 0.0 0.5 0.5 − 2.5 − − 2.5 − 2.0 − 1.5 − 1.0 − 0.5 − − − 0.0 0.5 − − − − − α α α LOG [OI] / H α α α α α LOG [OI] / H α α α LOG [OI] / H α α α α Models: Shocks V shocks = 100-300 km/s V shocks = 400-800 km/s N el : 100 and 1000 cm -3 s • Mild shocks associated to perturbation of the rotation • Strong shocks associated to non rotational motions β β − − − − − − − − − − − − − − − − − − − − − − − − − α α α − − − − − − − − − − − − − − − α α α
Optical spectroscopy of nearby type-1 LINERs Cazzoli et al. 2018 Optical Spectroscopy of local type-1 LINERs, Cazzoli+18 The AGN nature of L1 BLR elusive in ground based spectroscopy, ubiquitous in HST data AGN as the dominant mechanism of ionisation NLR stratification is often present The BLR-component detection and properties are sensitive to: template for H α -[NII] blend, number of Gaussians and starlight subtraction Kinematics and ionisation mechanism of the line components Narrow component: Rotation – all cases AGN photoionisation Second component: Non-rotational motions / outflows are frequent Associated to shocks ([OI] BPT + kinematics) The lack of neutral outflows might be a consequence of our classification Type-2 LINERs: Hermosa-Mu˜ noz+19 - POSTER Ongoing work 3D outflows and feedback with MEGARA/GTC and MUSE/VLT
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