The Physics and Physical Conditions of Quasar Outflows

The Physics and Physical Conditions of Quasar Outflows

Fred Hamann , Daniel Capellupo, George Chartas, Sean McGraw, Paola Rodriguez Hidalgo, Joseph Shields, Jane Charlton, Michael Eracleous
 University of Florida, Gainesville, Florida 32611, USA;  E-mail:fhamann@ufl.edu
Tel Aviv University, Tel Aviv, Israel
College of Charleston, Charleston, South Carolina, USA
Ohio University, Athens, Ohio, USA
York University, Toronto, Canada
Penn State University, State College, Pennsylvania, USA
Speaker.
Abstract

We describe two studies designed to characterize the total column densities, kinetic energies, and acceleration physics of broad absorption line (BAL) outflows in quasars. The first study uses new Chandra X-ray and ground-based rest-frame UV observations of 7 quasars with mini-BALs at extreme high speeds, in the range 0.1 to 0.2, to test the idea that strong radiative shielding (and therefore strong X-ray absorption) is needed to moderate the mini-BAL ionizations and facilitate their acceleration to extreme speeds. We find that the X-ray absorption is weak or absent, with generally cm, and that radiative shielding is not important. We argue that the mini-BAL ionizations are controlled, instead, by high gas densities of order cm in small outflow substructures. If we conservatively assume that the total column density in the mini-BAL gas is cm, covering 15% of the UV continuum source along our lines of sight (based on measured line depths), then the radial thickness of these outflows is only cm and their transverse size is cm. Thus the outflow regions have the shape of very thin “pancakes" viewed face-on, or they occupy larger volumes like a spray of dense cloudlets with a very small volume filling factor. We speculate that this situation (with ineffective shielding and small dense outflow substructures) applies to most quasar outflows, including BALs. Our second study focuses from BALs of low-abundance ions, mainly PV 1118,1128 Å, whose significant strengths imply large column densities, cm, that can further challenge models of the outflow acceleration. In spite of the difficulties of finding this line in the Ly forest, a search through the SDSS DR9 quasar catalog reveals 50 BAL sources at redshifts with strong PV BALs, which we are now using to characterize the general properties of high-column outflows.

The Physics and Physical Conditions of Quasar Outflows

 

Fred Hamannthanks: Speaker. , Daniel Capellupo, George Chartas, Sean McGraw, Paola Rodriguez Hidalgo, Joseph Shields, Jane Charlton, Michael Eracleous

University of Florida, Gainesville, Florida 32611, USA;  E-mail:fhamann@ufl.edu

Tel Aviv University, Tel Aviv, Israel

College of Charleston, Charleston, South Carolina, USA

Ohio University, Athens, Ohio, USA

York University, Toronto, Canada

Penn State University, State College, Pennsylvania, USA


\abstract@cs

The Extreme sky: Sampling the Universe above 10 keV - extremesky2009, November 6-8, 2012 Max-Planck-Insitut für Radioastronomie (MPIfR), Bonn, Germany

1 Introduction

Quasar outflows revealed by blueshifted broad absorption lines (BALs) are an important part of the quasar phenomenon. They are believed to be accelerated out from the atmospheres of quasar accretion disks by radiative forces, reaching observed speeds of a few thousand to tens of thousands of km s. While substantial progress has been made in our understanding of BAL outflows, important questions still remain their basic properties and acceleration physics. For example, it has long been known that the intense radiation available to drive quasar outflows can also over-ionize them and make them too transparent for radiative driving. This problem appeared to be solved by models that invoke a highly-ionized and radiatively thick “shield” at the base of the flows to protect the BAL gas from over-ionization and facilitate its acceleration to high speeds [11]. These models are supported by observations showing that BAL quasars are heavily absorbed in X-rays [6, 7]. However, this shielding picture runs into difficulty when we consider that the narrower cousins of BALs, the so-called mini-BALs, are not accompanied by strong X-ray absorption. They reach the same speeds with the same degrees of ionization as BALs without the benefits of a radiative shield.

In §2, we describe new observations and analyses of 7 mini-BAL quasars with extreme outflow speeds in the range 0.1 to 0.2 [10]. These are highly successful flows that must have favorable conditions for their acceleration. Our main goal is to test the hypothesis that high outflow speeds require a strong radiative shield. We show that the radiative shielding is negligible in these sources and, therefore, it is not important for the acceleration.

Another lingering problem is that measurements of the outflow column densities and kinetic energies are hampered by absorbing regions that only partially covering the background continuum source along our lines of sight. This can lead to absorption lines that do not reach zero intensity even if the line optical depths are orders of magnitude above unity. Section 3 presents early results from a program to find and measure BALs of rare ions, mainly PV 1118,1128 Å, that are signatures of large total column densities, cm, and extreme saturation in more commonly measured BALs like C iv 1548,1551 and O vi 1032,1038 [2].

2 Radiative Shielding in High-Velocity Mini-BAL Outflows

We selected 7 mini-BAL quasars with extreme outflow speeds ( km s) from our catalog of quasar outflow lines in the SDSS [12]. Figure 1 compares new rest-frame UV spectra obtained at the MDM observatory to earlier data from the SDSS or Lick Observatory (2001-2003). Chandra X-ray observations were obtained roughly concurrent with the MDM data (circa 2011). We find that most of the mini-BALs varied (Figure 1). This is consistent with the standard picture of mini-BALs belonging to the same general outflow phenomenon as BALs, close to the central black hole/accretion disk. The Chandra observations reveal weak or negligible amounts of X-ray absorption, with typically 0.0 to 0.1 and spectral fitting to the brightest individual source (also [13]) and joint fitting to the ensemble dataset indicating total X-ray column densities cm of neutral-equivalent absorption. These results are consistent with previous studies of lower-velocity mini-BALs that find X-ray absorbing columns at least an order of magnitude less than typical BAL quasars [8, 14].

Figure 1: Normalized MDM spectra in the quasar rest frames (red curves) overlaid on top of previous SDSS or Lick Observatory measurements (black curves) for the seven quasars in our mini-BAL sample. Significant mini-BALs are marked by red or black arrows in the MDM or previous spectra, respectively. Red arrows are not drawn if the mini-BAL disappeared or did not substantially change from the previous observation. The locations of several broad emission lines are shown across the top in the upper left panel.

We performed extensive photoionization simulations with the spectral synthesis code Cloudy [5] to determine the amounts of overall radiative shielding that might occur in these sources. These calculations are constrained by the observed weak X-ray absorption and weak or absent absorption lines in the UV (e.g., near velocity 0 where the shield is expected to reside). Table 1 and Figure 2 present the main results. The first three models listed in the table adopt a very large total column, cm, and large doppler parameters, to 1000 km s to maximize the shielding. The ionization parameter, , is adjusted to produce optical depth 0.1 in the C iv or O vi lines, consistent with the non-detections of these lines arising from the shield. These models can be ruled out because they produce too much X-ray absorption (Figure 1 and in Table 1). The fourth Cloudy model, called noC4b100xr, adopts a smaller total column density to be marginally consistent with both the UV and X-ray data.

— Line Optical Depths — —— HR ——
  Name C iv N v O vi Ne viii z=2.0 z=3.3  
Cloudy Models:
  noC4b100 23.5 2.11 100 0.1 2.5 226 365 4.8 2.9 -0.64
  noC4b1000 23.5 2.09 1000 0.1 0.9 36 56 5.1 3.0 -0.71
  noO6b1000 23.5 2.26 1000 0.1 3.5 3.0 2.4 -0.43
  noC4b1000xr 22.9 1.60 1000 0.2 1.3 47 76 2.5 1.8 -0.27
Neutral Absorbers:
  neutral22 22.0 1.5 1.2 -0.07
  neutral22.5 22.5 2.3 1.6 -0.23
  neutral23 23.0 4.1 2.5 -0.68

The column densities, , and doppler velocities, , have units cm and km s, respectively. The line optical depths apply to the short wavelength components of the doublets C iv 1548, N v 1239, O vi 1032, and Ne viii 770. Hardness ratios, HR, are listed for redshifts and . For comparison, the unabsorbed X-ray continuum used in these calculations, with , has HR = 0.85.

Table 1: Theoretical X-Ray Absorber/Shielding Results
Figure 2: Incident spectra (black curves) and transmitted spectra (blue curves) for the four Cloudy models listed in Table 1. The model names are given in the lower right of each panel. The bold red dashes connected by thin red dotted lines show the luminosities at 2500 Å (4.96 eV) and 2 keV used to calculate . Green curves in the lower right panel show transmitted X-ray spectra for the three neutral absorbers in Table 3, with , 22.5, and 23 cm from left to right. Ionization energies for some important ions are marked across the top. The observed Soft (0.2-2.0 keV) and Hard (2.0-10 keV) X-ray bands are shown by horizontal dashes for illustration at redshift . Small offsets of the transmitted spectra below the incident spectrum are due to electron scattering.

However, our main result is that these none of these quasars have significant radiative shielding because the putative absorbers do not block the far-UV radiation that can destroy important ions like C iv and O vi in the mini-BAL gas. This is evident from the weak absorption predicted near the ionization edges of these ions in Figure 1. Thus we find that while mini-BAL outflows reach the same speeds with the same moderate degrees of ionization as BAL outflows, they do so without the benefits of a radiative shield. We propose that the outflow ionizations are controlled, instead, by high gas densities defined by photoionization requirements to be

(2.0)

where the luminosity ergs s is roughly typical of our sample, pc is a reasonable guess for the location of the mini-BAL gas, and is an ionization parameter consistent with strong C iv and O vi mini-BALs. High gas densities then imply that the flows are like a fine spray, composed of many small substructures with a very small volume filling factor. These results support models like magnetic disk winds [4], that can confine small clouds with magnetic pressure and do not require a radiative shield for the acceleration.

3 PV & Large Outflow Column Densities

P v 1118,1128 is an important diagnostic of large column densities in BAL outflows [9, 1], but it can be difficult to measure in ground-based spectra because the short wavelengths require high redshift quasars that have severe Ly forest contamination below 1216 Å. We visually inspected 3000 BAL quasars in the SDSS DR9 with redshifts, , high enough to measure P v BALs. We find 50 quasars with definite strong P v BALs and many more quasars with P v BALs probably present. Figure 3 shows four quasars with strong P v BALs. We are presently working to characterize the BAL and broad emission line properties of this high column density sample, e.g., compared to other BAL and non-BAL quasar samples, and derive basic constraints on the outflow properties from photoionization analyses of the relative BAL strengths [2].

Figure 3: Rest-frame UV spectra of quasars from the SDSS3 DR9 that are representative of our sample with strong PV absorption [2]. Several prominent BALs are labeled by red dashed vertical lines.

References

  • [1] Borguet, B., et al. 2012, ApJ, 758, 69
  • [2] Capellupo, D., et al. 2013, in prep.
  • [3] Capellupo D., Hamann F., Shields J., Rodríguez Hidalgo P., Barlow T., 2012, MNRAS, in press
  • [4] de Kool M., Begelman M. C., 1995, ApJ, 455, 448
  • [5] Ferland G. J., et al. 1998, PASP, 110, 761
  • [6] Gallagher S. C., Brandt W. N., Chartas G., Garmire G. P., 2002, ApJ, 567, 37
  • [7] Gallagher S. C., et al. 2006, ApJ, 644, 709
  • [8] Gibson R. R., Brandt W. N., Gallagher S. C., Schneider D. P., 2009, ApJ, 696, 924
  • [9] Hamann F., 1998, ApJ, 500, 798
  • [10] Hamann, F., et al. 2013, in prep.
  • [11] Murray N., Chiang J., Grossman S. A., Voit G. M., 1995, ApJ, 451, 498
  • [12] Rodríguez Hidalgo, P. 2008, PhD dissertation, University of Florida
  • [13] Rodríguez Hidalgo P., Hamann F., Hall P., 2011, MNRAS, 411, 247
  • [14] Wu J., et al., 2010, ApJ, 724, 762
Comments 0
Request Comment
You are adding the first comment!
How to quickly get a good reply:
  • Give credit where it’s due by listing out the positive aspects of a paper before getting into which changes should be made.
  • Be specific in your critique, and provide supporting evidence with appropriate references to substantiate general statements.
  • Your comment should inspire ideas to flow and help the author improves the paper.

The better we are at sharing our knowledge with each other, the faster we move forward.
""
The feedback must be of minimum 40 characters and the title a minimum of 5 characters
   
Add comment
Cancel
Loading ...
169780
This is a comment super asjknd jkasnjk adsnkj
Upvote
Downvote
""
The feedback must be of minumum 40 characters
The feedback must be of minumum 40 characters
Submit
Cancel

You are asking your first question!
How to quickly get a good answer:
  • Keep your question short and to the point
  • Check for grammar or spelling errors.
  • Phrase it like a question
Test
Test description