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![Page 1: The AGN feedback process at work: does it suppress the star …adlibitum.oats.inaf.it/meetings/AGN11-Sept2014/Talks/B... · 2014-09-22 · disturbed [OIII] line profile) and the](https://reader034.pdfslide.us/reader034/viewer/2022050312/5f740d6b2a8acc0b980eae5b/html5/thumbnails/1.jpg)
Trieste -AGN11
BarbaraBalmaverde
Introduction
The sample
Properties ofthe [OIII] line
The starformation rate
Results
Conclusions &Discussions
The AGN feedback process at work:does it suppress the star formation rate
in local quasars?
Barbara Balmaverde
Universita di FirenzeDipartimento di Fisica e Astronomia
Coll: Alessandro Marconi
September 22, 2014
Barbara Balmaverde (Universita di Firenze) Trieste - AGN11 September 22, 2014 1 / 9
![Page 2: The AGN feedback process at work: does it suppress the star …adlibitum.oats.inaf.it/meetings/AGN11-Sept2014/Talks/B... · 2014-09-22 · disturbed [OIII] line profile) and the](https://reader034.pdfslide.us/reader034/viewer/2022050312/5f740d6b2a8acc0b980eae5b/html5/thumbnails/2.jpg)
Trieste -AGN11
BarbaraBalmaverde
Introduction
The sample
Properties ofthe [OIII] line
The starformation rate
Results
Conclusions &Discussions
Aim of the work:
Many theoretical models predict that AGN powerful outflows (commonly observed) are able to sweepaway the gas and stop the star formation in the host galaxy.From an observational point of view, there is strong connection between SFR and AGN luminosity.
Netzer et al. 2009; Shao et al. 2010 (see also Lutz
et al.2010, Mullaney et al. 2012, Rovilos et al. 2012,
Page et al. 2012, Harrison et al. 2012, Rosario et al.
2012)
Strong outflows are commonly observed, but are they effectively able to quench star formation?
Our aim is to explore the connection (if there is) between ionized gas outflows (probed bydisturbed [OIII] line profile) and the star formation rate of the galaxies in a sample of localquasars observed by Herschel.
Barbara Balmaverde (Universita di Firenze) Trieste - AGN11 September 22, 2014 2 / 9
![Page 3: The AGN feedback process at work: does it suppress the star …adlibitum.oats.inaf.it/meetings/AGN11-Sept2014/Talks/B... · 2014-09-22 · disturbed [OIII] line profile) and the](https://reader034.pdfslide.us/reader034/viewer/2022050312/5f740d6b2a8acc0b980eae5b/html5/thumbnails/3.jpg)
Trieste -AGN11
BarbaraBalmaverde
Introduction
The sample
Properties ofthe [OIII] line
The starformation rate
Results
Conclusions &Discussions
Aim of the work:
Many theoretical models predict that AGN powerful outflows (commonly observed) are able to sweepaway the gas and stop the star formation in the host galaxy.From an observational point of view, there is strong connection between SFR and AGN luminosity.
Netzer et al. 2009; Shao et al. 2010 (see also Lutz
et al.2010, Mullaney et al. 2012, Rovilos et al. 2012,
Page et al. 2012, Harrison et al. 2012, Rosario et al.
2012)
Strong outflows are commonly observed, but are they effectively able to quench star formation?
Our aim is to explore the connection (if there is) between ionized gas outflows (probed bydisturbed [OIII] line profile) and the star formation rate of the galaxies in a sample of localquasars observed by Herschel.
Barbara Balmaverde (Universita di Firenze) Trieste - AGN11 September 22, 2014 2 / 9
![Page 4: The AGN feedback process at work: does it suppress the star …adlibitum.oats.inaf.it/meetings/AGN11-Sept2014/Talks/B... · 2014-09-22 · disturbed [OIII] line profile) and the](https://reader034.pdfslide.us/reader034/viewer/2022050312/5f740d6b2a8acc0b980eae5b/html5/thumbnails/4.jpg)
Trieste -AGN11
BarbaraBalmaverde
Introduction
The sample
Properties ofthe [OIII] line
The starformation rate
Results
Conclusions &Discussions
The sample
THE SAMPLE: 226 quasars luminous unobscured (type 1) quasars from the qso catalogues of SDSS7
and SDSS10 with z < 1.0 observed in infrared by HERSCHEL.
AGN bolometric luminosity Redshift
Barbara Balmaverde (Universita di Firenze) Trieste - AGN11 September 22, 2014 3 / 9
![Page 5: The AGN feedback process at work: does it suppress the star …adlibitum.oats.inaf.it/meetings/AGN11-Sept2014/Talks/B... · 2014-09-22 · disturbed [OIII] line profile) and the](https://reader034.pdfslide.us/reader034/viewer/2022050312/5f740d6b2a8acc0b980eae5b/html5/thumbnails/5.jpg)
Trieste -AGN11
BarbaraBalmaverde
Introduction
The sample
Properties ofthe [OIII] line
The starformation rate
Results
Conclusions &Discussions
Fit to the optical lines
The [OIII] line is a good diagnostic of outflows at large scale.The [OIII] line generally reveals complex motion in the NLR (e.g. Broad blue wings...)
Barbara Balmaverde (Universita di Firenze) Trieste - AGN11 September 22, 2014 4 / 9
![Page 6: The AGN feedback process at work: does it suppress the star …adlibitum.oats.inaf.it/meetings/AGN11-Sept2014/Talks/B... · 2014-09-22 · disturbed [OIII] line profile) and the](https://reader034.pdfslide.us/reader034/viewer/2022050312/5f740d6b2a8acc0b980eae5b/html5/thumbnails/6.jpg)
Trieste -AGN11
BarbaraBalmaverde
Introduction
The sample
Properties ofthe [OIII] line
The starformation rate
Results
Conclusions &Discussions
Fit to the optical lines
We fit the line with a broad and a narrow component, but to characterize the outflow we adopt a nonparametric definition for the velocity. For example:
Broad Offset velocity = v05+v952
(e.g. Harrison et al.2014)
Max projected velocity = vel98 − vel02
Velocity Reference: the [OII] emission line trace the quiet gas on large scale.
−2000 −1000 0 1000 20000
1•1040
2•1040
3•1040
4•1040
5•1040
6•1040
−2000 −1000 0 1000 2000Velocity [km s−1]
0
1•1040
2•1040
3•1040
4•1040
5•1040
6•1040
Lum
inos
ity [a
.u.]
v02
v05
v50
v95
v98
Barbara Balmaverde (Universita di Firenze) Trieste - AGN11 September 22, 2014 5 / 9
![Page 7: The AGN feedback process at work: does it suppress the star …adlibitum.oats.inaf.it/meetings/AGN11-Sept2014/Talks/B... · 2014-09-22 · disturbed [OIII] line profile) and the](https://reader034.pdfslide.us/reader034/viewer/2022050312/5f740d6b2a8acc0b980eae5b/html5/thumbnails/7.jpg)
Trieste -AGN11
BarbaraBalmaverde
Introduction
The sample
Properties ofthe [OIII] line
The starformation rate
Results
Conclusions &Discussions
QSO infrared luminosities
Herschel observe in the optimal wavelength range to measure the “cold” emission of the dust heatedby young stars.
Barbara Balmaverde (Universita di Firenze) Trieste - AGN11 September 22, 2014 6 / 9
![Page 8: The AGN feedback process at work: does it suppress the star …adlibitum.oats.inaf.it/meetings/AGN11-Sept2014/Talks/B... · 2014-09-22 · disturbed [OIII] line profile) and the](https://reader034.pdfslide.us/reader034/viewer/2022050312/5f740d6b2a8acc0b980eae5b/html5/thumbnails/8.jpg)
Trieste -AGN11
BarbaraBalmaverde
Introduction
The sample
Properties ofthe [OIII] line
The starformation rate
Results
Conclusions &Discussions
The star formation rate
Disantangle the contribution from the AGN and from star-forming regions is not easy, expecially forpowerful Type 1 quasars. We rely on clumpy torus templates by Nenkova et al. 2008 and starbursttemplates by Charlot&Elbaz 2001.
SFRFIR(M⊙ yr−1) = (4.5× 10−44)LFIR erg s−1
Kennicutt et al. 1998
Barbara Balmaverde (Universita di Firenze) Trieste - AGN11 September 22, 2014 7 / 9
![Page 9: The AGN feedback process at work: does it suppress the star …adlibitum.oats.inaf.it/meetings/AGN11-Sept2014/Talks/B... · 2014-09-22 · disturbed [OIII] line profile) and the](https://reader034.pdfslide.us/reader034/viewer/2022050312/5f740d6b2a8acc0b980eae5b/html5/thumbnails/9.jpg)
Trieste -AGN11
BarbaraBalmaverde
Introduction
The sample
Properties ofthe [OIII] line
The starformation rate
Results
Conclusions &Discussions
The star formation rate
Disantangle the contribution from the AGN and from star-forming regions is not easy, expecially forpowerful Type 1 quasars. We rely on clumpy torus templates by Nenkova et al. 2008 and starbursttemplates by Charlot&Elbaz 2001.
SFRFIR(M⊙ yr−1) = (4.5× 10−44)LFIR erg s−1
Kennicutt et al. 1998
Barbara Balmaverde (Universita di Firenze) Trieste - AGN11 September 22, 2014 7 / 9
![Page 10: The AGN feedback process at work: does it suppress the star …adlibitum.oats.inaf.it/meetings/AGN11-Sept2014/Talks/B... · 2014-09-22 · disturbed [OIII] line profile) and the](https://reader034.pdfslide.us/reader034/viewer/2022050312/5f740d6b2a8acc0b980eae5b/html5/thumbnails/10.jpg)
Trieste -AGN11
BarbaraBalmaverde
Introduction
The sample
Properties ofthe [OIII] line
The starformation rate
Results
Conclusions &Discussions
What we found?
We divided our sample in two groups: the first one is composed by star-burst dominated objects, forwhich the starburst luminosity component dominates the total infrared (8-1000 µm ) luminosity(LSB /Ltot >0.5) and the second group is composed by AGN dominated objects (LSB /Ltot <0.5).
Balmaverde et al. IN PREPARATION
500 1000 1500 2000 2500 3000
0
1
2
3
4
500 1000 1500 2000 2500 3000(V98−V02) [km s−1]
0
1
2
3
4
log
SF
R [M
sun y
r−1 ]
500 1000 1500 2000 2500 3000
0
1
2
3
4
500 1000 1500 2000 2500 3000(V98−V02) [km s−1]
0
1
2
3
4
log
SF
R [M
sun y
r−1 ]
r= 0.45
Barbara Balmaverde (Universita di Firenze) Trieste - AGN11 September 22, 2014 8 / 9
![Page 11: The AGN feedback process at work: does it suppress the star …adlibitum.oats.inaf.it/meetings/AGN11-Sept2014/Talks/B... · 2014-09-22 · disturbed [OIII] line profile) and the](https://reader034.pdfslide.us/reader034/viewer/2022050312/5f740d6b2a8acc0b980eae5b/html5/thumbnails/11.jpg)
Trieste -AGN11
BarbaraBalmaverde
Introduction
The sample
Properties ofthe [OIII] line
The starformation rate
Results
Conclusions &Discussions
What we found?
We divided our sample in two groups: the first one is composed by star-burst dominated objects, forwhich the starburst luminosity component dominates the total infrared (8-1000 µm ) luminosity(LSB /Ltot >0.5) and the second group is composed by AGN dominated objects (LSB /Ltot <0.5).
Balmaverde et al. IN PREPARATION
500 1000 1500 2000 2500 3000
0
1
2
3
4
500 1000 1500 2000 2500 3000(V98−V02) [km s−1]
0
1
2
3
4
log
SF
R [M
sun y
r−1 ]
500 1000 1500 2000 2500 3000
0
1
2
3
4
500 1000 1500 2000 2500 3000(V98−V02) [km s−1]
0
1
2
3
4
log
SF
R [M
sun y
r−1 ]
r= 0.45
Barbara Balmaverde (Universita di Firenze) Trieste - AGN11 September 22, 2014 8 / 9
![Page 12: The AGN feedback process at work: does it suppress the star …adlibitum.oats.inaf.it/meetings/AGN11-Sept2014/Talks/B... · 2014-09-22 · disturbed [OIII] line profile) and the](https://reader034.pdfslide.us/reader034/viewer/2022050312/5f740d6b2a8acc0b980eae5b/html5/thumbnails/12.jpg)
Trieste -AGN11
BarbaraBalmaverde
Introduction
The sample
Properties ofthe [OIII] line
The starformation rate
Results
Conclusions &Discussions
Conclusions & Discussions
We selected powerful Type1 quasars at z < 1.0 and we do not see any connection between outflowproperties and SFR IF WE CONSIDER AGN AND SB DOMINATED OBJECTS TOGETHER.
However, if we consider only the SF-dominated objects (blue points) a positive correlation emerges.Stellar origin for the winds in SB dominated quasars?
In the AGN dominated quasars we do not see any relation between OUTFLOW and SFR. Why?
AGN feedback affects only in the central region of the galaxy.
Positive and negative feedback effects are mixed.
The QSO active phase timescale is shorter (≪ Myr) than the time to switch off the hot stars
which heat the dust (∼ Ten(s) of Myr e.g Hopkins et al.
Barbara Balmaverde (Universita di Firenze) Trieste - AGN11 September 22, 2014 9 / 9
![Page 13: The AGN feedback process at work: does it suppress the star …adlibitum.oats.inaf.it/meetings/AGN11-Sept2014/Talks/B... · 2014-09-22 · disturbed [OIII] line profile) and the](https://reader034.pdfslide.us/reader034/viewer/2022050312/5f740d6b2a8acc0b980eae5b/html5/thumbnails/13.jpg)
Trieste -AGN11
BarbaraBalmaverde
Introduction
The sample
Properties ofthe [OIII] line
The starformation rate
Results
Conclusions &Discussions
Conclusions & Discussions
We selected powerful Type1 quasars at z < 1.0 and we do not see any connection between outflowproperties and SFR IF WE CONSIDER AGN AND SB DOMINATED OBJECTS TOGETHER.
However, if we consider only the SF-dominated objects (blue points) a positive correlation emerges.Stellar origin for the winds in SB dominated quasars?
In the AGN dominated quasars we do not see any relation between OUTFLOW and SFR. Why?
AGN feedback affects only in the central region of the galaxy.
Positive and negative feedback effects are mixed.
The QSO active phase timescale is shorter (≪ Myr) than the time to switch off the hot stars
which heat the dust (∼ Ten(s) of Myr e.g Hopkins et al.
Barbara Balmaverde (Universita di Firenze) Trieste - AGN11 September 22, 2014 9 / 9
![Page 14: The AGN feedback process at work: does it suppress the star …adlibitum.oats.inaf.it/meetings/AGN11-Sept2014/Talks/B... · 2014-09-22 · disturbed [OIII] line profile) and the](https://reader034.pdfslide.us/reader034/viewer/2022050312/5f740d6b2a8acc0b980eae5b/html5/thumbnails/14.jpg)
Trieste -AGN11
BarbaraBalmaverde
Introduction
The sample
Properties ofthe [OIII] line
The starformation rate
Results
Conclusions &Discussions
Conclusions & Discussions
We selected powerful Type1 quasars at z < 1.0 and we do not see any connection between outflowproperties and SFR IF WE CONSIDER AGN AND SB DOMINATED OBJECTS TOGETHER.
However, if we consider only the SF-dominated objects (blue points) a positive correlation emerges.Stellar origin for the winds in SB dominated quasars?
In the AGN dominated quasars we do not see any relation between OUTFLOW and SFR. Why?
AGN feedback affects only in the central region of the galaxy.
Positive and negative feedback effects are mixed.
The QSO active phase timescale is shorter (≪ Myr) than the time to switch off the hot stars
which heat the dust (∼ Ten(s) of Myr e.g Hopkins et al.
Barbara Balmaverde (Universita di Firenze) Trieste - AGN11 September 22, 2014 9 / 9
![Page 15: The AGN feedback process at work: does it suppress the star …adlibitum.oats.inaf.it/meetings/AGN11-Sept2014/Talks/B... · 2014-09-22 · disturbed [OIII] line profile) and the](https://reader034.pdfslide.us/reader034/viewer/2022050312/5f740d6b2a8acc0b980eae5b/html5/thumbnails/15.jpg)
Trieste -AGN11
BarbaraBalmaverde
Introduction
The sample
Properties ofthe [OIII] line
The starformation rate
Results
Conclusions &Discussions
Conclusions & Discussions
We selected powerful Type1 quasars at z < 1.0 and we do not see any connection between outflowproperties and SFR IF WE CONSIDER AGN AND SB DOMINATED OBJECTS TOGETHER.
However, if we consider only the SF-dominated objects (blue points) a positive correlation emerges.Stellar origin for the winds in SB dominated quasars?
In the AGN dominated quasars we do not see any relation between OUTFLOW and SFR. Why?
AGN feedback affects only in the central region of the galaxy.
Positive and negative feedback effects are mixed.
The QSO active phase timescale is shorter (≪ Myr) than the time to switch off the hot stars
which heat the dust (∼ Ten(s) of Myr e.g Hopkins et al.
Barbara Balmaverde (Universita di Firenze) Trieste - AGN11 September 22, 2014 9 / 9
![Page 16: The AGN feedback process at work: does it suppress the star …adlibitum.oats.inaf.it/meetings/AGN11-Sept2014/Talks/B... · 2014-09-22 · disturbed [OIII] line profile) and the](https://reader034.pdfslide.us/reader034/viewer/2022050312/5f740d6b2a8acc0b980eae5b/html5/thumbnails/16.jpg)
Trieste -AGN11
BarbaraBalmaverde
Introduction
The sample
Properties ofthe [OIII] line
The starformation rate
Results
Conclusions &Discussions
Conclusions & Discussions
We selected powerful Type1 quasars at z < 1.0 and we do not see any connection between outflowproperties and SFR IF WE CONSIDER AGN AND SB DOMINATED OBJECTS TOGETHER.
However, if we consider only the SF-dominated objects (blue points) a positive correlation emerges.Stellar origin for the winds in SB dominated quasars?
In the AGN dominated quasars we do not see any relation between OUTFLOW and SFR. Why?
AGN feedback affects only in the central region of the galaxy.
Positive and negative feedback effects are mixed.
The QSO active phase timescale is shorter (≪ Myr) than the time to switch off the hot stars
which heat the dust (∼ Ten(s) of Myr e.g Hopkins et al.
Barbara Balmaverde (Universita di Firenze) Trieste - AGN11 September 22, 2014 9 / 9
![Page 17: The AGN feedback process at work: does it suppress the star …adlibitum.oats.inaf.it/meetings/AGN11-Sept2014/Talks/B... · 2014-09-22 · disturbed [OIII] line profile) and the](https://reader034.pdfslide.us/reader034/viewer/2022050312/5f740d6b2a8acc0b980eae5b/html5/thumbnails/17.jpg)
Trieste -AGN11
BarbaraBalmaverde
Introduction
The sample
Properties ofthe [OIII] line
The starformation rate
Results
Conclusions &Discussions
Conclusions & Discussions
We selected powerful Type1 quasars at z < 1.0 and we do not see any connection between outflowproperties and SFR IF WE CONSIDER AGN AND SB DOMINATED OBJECTS TOGETHER.
However, if we consider only the SF-dominated objects (blue points) a positive correlation emerges.Stellar origin for the winds in SB dominated quasars?
In the AGN dominated quasars we do not see any relation between OUTFLOW and SFR. Why?
AGN feedback affects only in the central region of the galaxy.
Positive and negative feedback effects are mixed.
The QSO active phase timescale is shorter (≪ Myr) than the time to switch off the hot stars
which heat the dust (∼ Ten(s) of Myr e.g Hopkins et al.
Barbara Balmaverde (Universita di Firenze) Trieste - AGN11 September 22, 2014 9 / 9
![Page 18: The AGN feedback process at work: does it suppress the star …adlibitum.oats.inaf.it/meetings/AGN11-Sept2014/Talks/B... · 2014-09-22 · disturbed [OIII] line profile) and the](https://reader034.pdfslide.us/reader034/viewer/2022050312/5f740d6b2a8acc0b980eae5b/html5/thumbnails/18.jpg)
Trieste -AGN11
BarbaraBalmaverde
Introduction
The sample
Properties ofthe [OIII] line
The starformation rate
Results
Conclusions &Discussions
Conclusions & Discussions
We selected powerful Type1 quasars at z < 1.0 and we do not see any connection between outflowproperties and SFR IF WE CONSIDER AGN AND SB DOMINATED OBJECTS TOGETHER.
However, if we consider only the SF-dominated objects (blue points) a positive correlation emerges.Stellar origin for the winds in SB dominated quasars?
In the AGN dominated quasars we do not see any relation between OUTFLOW and SFR. Why?
AGN feedback affects only in the central region of the galaxy.
Positive and negative feedback effects are mixed.
The QSO active phase timescale is shorter (≪ Myr) than the time to switch off the hot stars
which heat the dust (∼ Ten(s) of Myr e.g Hopkins et al.
Barbara Balmaverde (Universita di Firenze) Trieste - AGN11 September 22, 2014 9 / 9
![MNRAS ATEX style le v3 · 2019. 5. 21. · MNRAS 000,1{14(2019) Preprint 21 May 2019 Compiled using MNRAS LATEX style le v3.0 [Oiii] Emission Line Properties in a New Sample of Heavily](https://img.pdfslide.us/doc/110x75/60551c0eb3cc4f2e05089780/mnras-atex-style-le-v3-2019-5-21-mnras-0001142019-preprint-21-may-2019.jpg)
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![Obscured AGNs in Advanced Mergershiddenmonsters/talks/satyapal.pdf · Satyapal et al. (2014) Measured in the optical with [OIII]: Ellison et al. (2013) Obscured Phase Occurs at Peak](https://img.pdfslide.us/doc/110x75/602aeca30c5eed0cb36b1975/obscured-agns-in-advanced-mergers-hiddenmonsterstalkssatyapalpdf-satyapal-et.jpg)
![Spectral Range and Resolution Huan Lin Fermilab. 2 Wavelengths5500 Å6000 Å10000 Å Emission line redshifts [OII] 37270.480.611.68 [OIII] 50070.100.201.00](https://img.pdfslide.us/doc/110x75/56649d7b5503460f94a5f58e/spectral-range-and-resolution-huan-lin-fermilab-2-wavelengths5500-a6000-a10000.jpg)
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![The width of the [OIII]5007 emission line and its](https://img.pdfslide.us/doc/110x75/61cc47f29cc0121b7a773a9a/the-width-of-the-oiii5007-emission-line-and-its-.jpg)
