Investigation of Radio Structures of High-z QSOs by VLBI Observation

Transcription

1 Investigation of Radio Structures of High-z QSOs by VLBI Observation

2 Challenges of 512 Frey et al.: High resolution radio imaging parsec-scale jet component speeds (Fig. 4). More radio luminous sources have faster jets. Both the radios.powers and Fig GHz extended lum jet speeds vary smoothly between the BL Lac and quasar subclasses. Therefore, at least in terms of radio jet AGN jets 1/2/217 circles denote quasars and BL properties, the BL Lacs and quasars do not appear to be distinctly different. galaxies. Core-only sources a INTRODUCTION Relationship to Large-scale Environment As there have been suggestions that the lobe power is affected by jet-environment interactions on kpc-scales, we have defined the ratio of the lobe radio power to the blazar absolute optical magnitude to be a proxy for environmental effects. This ratio is correlated with redshift, as expected (e.g., Best et al., 1999, MNRAS, 33; see Fig. 5). While the sources with FRI powers appear to be at lower redshifts, the FRII and FRI/II sources show a similar distribution, suggesting that environmental differences are not crucial in determining the total radio power in these Big sources (Fig. 6). This ratio does not correlate with jet speeds, suggesting that factors intrinsic to the AGN, or the local parsec-scale enviornment influence the jets speeds, and thereby the Bang extended radio power. Fig. 5. The environment indicator proxy versus redshift. (Left) Open and fi 13.7 billion year respectively, while open squares denote radio galaxies. Core-only sources divided on the basis of extended radio luminosity into FRI (=1), FRII (=2), Chandra Observations of MOJAVE blaza Of the MOJAVE blazars with significant extended radio emission, nea in our ~1 ks Chandra observations (Hogan et al., in preparation), indic relativistic bulk motion in producing X-ray emission. As a followup to t were awarded ~7 ks of time on the Chandra telescope for observing 16+13, and The observations for took place is scheduled to be observed next month Preliminary Findings The highly polarized quasar lies at a redshift of 2.99 (1" = ~38 kpc radio jet is one-sided, suggesting a highly relativistic jet on kp line of sight (Fig. 6, Left). Its highest parsec-scale jet component spee few high apparent jet speed source in the MOJAVE sample. High-z QSOs are similar structures to Low-z ones. The Innermost Regions of Relativistic Jets and Their Magnetic Fields Relative Decl. (mas) Preeti Kharb, Matthew Lister Peak: mjy beam 1 p Contours:.4 2 mjy beam 1 Fig. 6. (Left) The 4.9 GHz radio image of (Center) The Chandra.5 7 kev filtered image (in colour) with the 4.9 GHz radio contours and (Right) 8.4 GHz radio contours superimposed. 15 The data were reduced and analysed using the CIAO software versio (CALDB) version After reprocessing the level 1 events file (to re randomization) and creating a new level 2 file, we used the CIAO tool L.I. 7. kev)2filtered image to get flux estimates. The core and et jetal.flux valu S. Frey 2 2 ergs/cm /s and 1.5E-13 ergs/cm /s, respectively. X-ray spectral fitting analysed. As seen in Fig. 6, the X-ray jet follows the radio jet remarka Fig. 1a d. 5 GHz images of a , b , c and d 15 bend just like the radio jet, and seems to terminate just before the rad of the peak brightness of 162 mjy/beam; restoring beam is mas at PA= brightness of 886 mjy/beam; restoring beam is mas at PA=21 ; c.2 This work partially restoring supported byisnasa grant 87ismJy/beam; beam mas G9-128X. at PA=16 ; d.25,.25,.5, 1 restoring beam is mas at PA= Observations, calibration and data reduction Joseph et al. The source coordinates, redshifts and total flux densities are shown in Table 1. All observations were made at 5 GHz using left circular polarization. Bonn in Tab Fr AIPS plitud sured

3 Challenges of AGN jets 1/2/217 INTRODUCTION However No GPS and CSO sources are found at low-z. 2 mas VLBI image of CSO SED of GPS source J. D. Collier et al.

4 Challenges of AGN jets 1/2/217 MOTIVATION Observing the high-z QSOs may provide constraints on the models of their birth and early cosmological evolution, the growth of the central SMBHs, the onset of AGN activity period in the radio band. Only ~2 VLBI images of high-z QSOs are available. (Frey et al.) Few statistical discussions CSO like More VLBI images of high-z QSOs are required. Morphological Study on High-z QSOs core-jet like

5 Challenges of AGN jets 1/2/217 SOURCE SELECTION Selection Criteria Flux > 3 mjy at 1.4 GHz from FIRST catalog z > 4 from SDSS catalog JVN sensitivity ~1 mjy at 8.4 GH (32 MHz bandwidth). taking into account the typical spectral index of -.5 of high-z radio QSOs. We selected 13 objects satisfying these conditions.

6 Challenges of AGN jets 1/2/217 PREVIOUS STUDY 6 sources were already observed. 2 of 6 were detected. JVN Non-detected Detected Non-detected Freq.: 8.4 GHz (32MHz bandwidth)

7 Challenges of AGN jets 1/2/217 1 Peak flux= Jy/beam map rms= Jy/beam Peak flux= Jy/beam map rms= Jy/beam J mas -1-2 J mas Non-detected Detected Non-dete

8 Challenges of AGN jets 1/2/217 NEW OBSERVATION Period : 216/9/29 22:45-9/3 9:45 (UT) Freq. : MHz (512 MHz bandwidth) Pol. : RHCP New Observation

9 Challenges of AGN jets 1/2/217 NEW OBSERVATION Period The : 216/9/29 amplifiers 22:45 at - 9/3 9:45 (UT) Freq. : MHz (512 MHz bandwidth) Mizusawa, Ishigaki and Ogasawara were broken, Pol. : RHCP so I observed only by 4 telescopes. New Observation

10 Challenges of AGN jets 1/2/217 RESULT&DISCUSSION We could detect without phase reference We detected the flux of <1mJy!! PLot file version 1 created 24-DEC :32:35 BOTH: IPOL MHz ICL PLot file version 1 created 24-DEC :34:53 BOTH: IPOL MHz ICL PLot file version 1 created 24-DEC :57:22 BOTH: IPOL MHz ICL Peak flux= Jy/beam map rms= Jy/beam 5 4 Peak flux= Jy/beam map rms= Jy/beam 15 1 Peak flux= Jy/beam map rms= Jy/beam mas -4 2mas -1 5mas Center at RA DEC Grey scale flux range= MilliJY/BEAM Cont peak flux = E-2 JY/BEAM Levs = 1.1E-3 * (6, 8, 1, 12, 14, 16, 18, 2) Center at RA DEC Grey scale flux range= MilliJY/BEAM Cont peak flux = E-2 JY/BEAM Levs = 1.3E-3 * (6, 8, 1, 12, 14, 16, 18, 2) Center at RA DEC Grey scale flux range= MilliJY/BEAM Cont peak flux = E-3 JY/BEAM Levs = 3.5E-4 * (6, 8, 1, 12, 14, 16, 18, 2) J J J The size of all targets are much smaller than synthesized beam.

11 Challenges of AGN jets 1/2/217 SUMMARY&FUTURE The size of all targets are much smaller than synthesized beams. PLot file version 1 created 24-DEC :34:53 BOTH: IPOL MHz ICL PLot file version 1 created 24-DEC :32:35 BOTH: IPOL MHz ICL PLot file version 1 created 24-DEC :57:22 BOTH: IPOL MHz ICL PLot file version 2 created 24-DEC :25: BOTH: J IPOL MHz J ICL PLot file version 3 created 25-DEC-216 :23:32 BOTH: J IPOL MHz J ICL Center at RA DEC Grey scale flux range= MilliJY/BEAM Cont peak flux = E-2 JY/BEAM Levs = 1.3E-3 * (6, 8, 1, 12, 14, 16, 18, 2) Center at RA DEC Grey scale flux range= MilliJY/BEAM Cont peak flux = E-2 JY/BEAM Levs = 1.1E-3 * (6, 8, 1, 12, 14, 16, 18, 2) Center at RA DEC Grey scale flux range= MilliJY/BEAM Cont peak flux = E-3 JY/BEAM Levs = 3.5E-4 * (6, 8, 1, 12, 14, 16, 18, 2) Center at RA DEC Grey scale flux range= MilliJY/BEAM Cont peak flux = E-1 JY/BEAM Levs = 5.9E-2 * (2, 2.5, 3, 3.5, 4, 4.5, 5, 5.5) Center at RA DEC Grey scale flux range= MilliJY/BEAM Cont peak flux = E-2 JY/BEAM Levs = 6.6E-3 * (6, 8, 1, 12, 14, 16, 18, 2) J J J J J We haven t observed 4 sources yet. Yet Yet Yet

12 THANK YOU!!