# agn06.ihep.ac.cnmainpresentationsPaolaRodriguez by dfhdhdhdhjr

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```									High Velocity Outflows
in Quasars
Paola Rodriguez Hidalgo
University of Florida
Collaborators: Daniel Nestor,
Joseph Shields
Classification of Absorption Lines
 Based on similar redshift to the quasar:
Associated
Non-associated
 Based on the absorber is ejected from the quasar:
Intrinsic
Non-intrinsic
 Based on the width of the line:
BAL
NAL
miniBAL
Classification of Absorption Lines
 Based on similar redshift to the quasar:
Associated
Non-associated               High Velocity
 Based on the absorber is ejected from the quasar:
Intrinsic                  Outflows
Non-intrinsic
 Based on the width of the line:
BAL: form in winds
NAL: origin? Most AALs are intrinsic (see Leah Simon,
Daniel Nestor and Rajib Ganguly posters), how many at High
Velocity (HV) are intrinsic? (36% ? - Richards et al. 1999,
2001)
miniBAL: barely studied: how common are they?, how
often do they appear at HV?
Example of a
High Velocity Outflow
Ly+NV               PG 0935+417

v ~ 51,000 km/s
SiIV+OIV          CIV

CIV!
Goals
1) Account for types of outflows to input
information into physical/geometrical
models.
2) Understand miniBAL-BAL relationship:
distinct or same thing with different
sightline?
3) Confirm intrinsic nature of large number of
systems for follow-up and, hopefully, get
information about location, densities, … and
to explain wind structure and dynamics.
Searching for High Velocity
Outflows: the Sample
 SDSS Quasar spectra:
 R ~ 150 km/s
 Spectral coverage 3820-9200 A;
to see CIV 1548,1550 absorbers: zem > 1.8
to see velocities up to 0.2c:        zem > 2.1
 Choose the n(t) spectra with best S/N
 Look for every blue-shifted CIV absorber
- zabs, v, FWHM, REW, BI, AI
Searching for High Velocity
Outflows: the Sample
 SDSS Quasar spectra:
 R ~ 150 km/s
 Spectral coverage 3820-9200 A;
to see CIV 1548,1550 absorbers: zem > 1.8
to see velocities up to 0.2c:        zem > 2.1
 Choose the 2,200 spectra with best S/N -> 1,846
 Look for every blue-shifted CIV absorber
- zabs, v, FWHM, REW, BI, AI
- 5320 absorption systems measured
.11   17.13   17.08   16.80   16.71   02:08:45.54    00:22:36.07   1.885   1.677   22502   1551   0.61   0.43
.95   17.46   17.08   16.95   16.80   12:05:50.19    02:01:31.58   2.133   1.964   16108   6077   2.82   1.42
.66
.56
17.36
17.23   Searching for High Velocity
17.09
17.09
17.01
16.97
16.85
16.90
13:28:01.25
16:55:42.60
57:31:13.09
38:13:38.36
2.057
1.906
1.657
1.509
41774
43746
2800
2482
1.89
0.81
0.95
0.81

Outflows: the results
.63   17.43   17.21   17.07   16.91   14:41:05.53    04:54:54.95   2.064   1.543   55229   4243   3.66   1.90
.63   17.43   17.21   17.07   16.91   14:41:05.53    04:54:54.95   2.064   1.618   46772   2381   1.01   0.51
.35   17.31   17.27   17.09   17.02   10:31:12.24    38:07:17.23   1.893   1.684   22480    986   0.44   0.44
.21   17.82   17.28   16.84   16.76   14:37:52.76    04:28:54.54   1.919   1.733   19702   3849   3.52   1.88
.23   17.56   17.30   17.25   16.94   11:13:13.29    10:22:12.45   2.247   2.026   20884    992   1.44   1.44
.62   17.50   17.38   17.27   17.04   13:48:55.28   -03:21:41.41   2.099   1.550   57766   1592   0.96   0.96
.95   17.86   17.42   16.97   16.97   08:10:33.57    23:32:23.10   1.869   1.739   11233   5609   4.57   2.29
.40   17.78   17.45   17.46   17.33   09:46:46.94    39:27:19.02   2.207   1.815   38878   2619   2.82   2.84
.06   17.61   17.49   17.49   17.28   10:43:30.09    44:10:51.61   2.209   1.980   22136   2264   2.32   1.17
.77   17.62   17.53   17.40   17.13   14:22:46.59    35:28:36.02   2.105   1.921   18303   1944   1.56   1.56
.74   17.59   17.55   17.32   17.32   10:01:28.61    50:27:56.90   1.839   1.765    7589   2709   1.88   1.91
.02   17.79   17.55   17.45   17.27   16:15:11.36    31:47:28.35   2.095   1.764   33705   3713   2.73   2.75
.02   17.79   17.55   17.45   17.27   16:15:11.36    31:47:28.35   2.095   1.874   22175   1341   1.75   0.88
.82   17.64   17.59   17.45   17.37   14:16:44.39    44:15:57.39   1.921   1.718   21537   1545   0.58   0.58
.10   17.70   17.61   17.43   17.16   15:45:50.38    55:43:46.23   2.156   1.985   17315    984   0.87   0.82
.36   17.87   17.65   17.61   17.47   08:58:56.01    01:52:19.41   2.158   1.912   24195   1174   0.68   0.34
.13   17.85   17.65   17.52   17.38   08:31:04.90    53:25:00.17   2.065   1.963    9787   1233   2.30   1.15
.95   17.79   17.66   17.44   17.45   12:43:12.94    14:48:12.10   1.860   1.709   16319   1182   0.72   0.72
CIV absorbers found

Restframe wavelength (A)
CIV absorbers found
• Number of miniBALs = 423
• Number of quasars with miniBALs =
284
• Number of quasars with miniBALs at
v > 10,000 km s-1 = 175
• Number of quasars with miniBALs at
v > 25,000 km s-1 = 51
CIV absorbers found
14%

2.5%
Some questions:
 What sorts of structures and what lines of
sight through the outflow produce miniBALs?
 How often should we see miniBALs vs BALs
and NALs if we view these outflows along
random sightlines?
 How fast do miniBALs evolve or cross the line
of sight? Should we see acceleration
/decceleration?
 Should HV miniBALs come with more/less
Xray abs than BALs?
Variability study
Ly+NV               PG 0935+417

v ~ 51,000 km/s
SiIV+OIV          CIV

CIV!
Variability study

HV CIV

Observed wavelength (A)
Searching for Variability: Data
 KPNO 2.1m :    R~200 km s-1, ~3600-6200 A
 MDM 2.4m : R~230 km s-1 , ~3600-5200 A
(collaboration with Joe Shields)
 Lick 3.0m : (collaboration with Jason
 Literature: LBQS survey (Hewitt et al. 1994),
etc…
Variability study: some results
Variability study: some results
• 18 well-measured quasars in 3 observing campaigns
• 5 quasars show clear variability in miniBALs
(5/18~30%):
If changes are due to ionization:
tobs=0.7-1.9 yrs = high (?) upper limit for tvar
ne= 6000-16200 cm-3 : lower limit
Rmax=1700-4900 pc : upper limit
• So far, no variability in NALs
• Most systems vary only in strength, but some show
shift in velocities
Current & Future work
 Continue Variability study ->looking for more
intrinsic systems and monitoring campaign to
study flow properties of confirmed ones
 High resolution observations of
best/interesting candidates to obtain more
accurate properties
 Compare to absorption in Xray data to
explore UV-Xray correlations and the
relationship miniBALs-BALs
 Input results in current theoretical models to
help constrain parameters
Summary
 We have searched the SDSS database looking for CIV
absorbers to compile, for the first time, a catalog of
CIV absorption lines in high-redshift quasars: 2,200
quasars, 5320 CIV absorption systems found
 We did and continue to follow up some of these
systems with new observations (KPNO 2.1m,
MDM 2.4m, Lick 3.0m) to confirm intrinsic nature
based on variability and characterize it.
 We will follow up with Xray observations to study the
relationship UV-Xray absorbers and miniBALs-BALs.
 We will input the results into theoretical models to
help constrain model parameters.

Xiexie
Questionable/Interesting HV
candidates

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