Abstract
We report the initial results of an adaptive-optics-assisted, optical integral-field-unit observation of IRAS 04576+0912, the nearest (z = 0.039) active galactic nucleus with a prominent ...blueshift/tail in O iii emission from a sample of such objects that we have collected from the literature. We aim at addressing the putative quasar-mode feedback process with Subaru/Kyoto 3D II+AO188. The optical waveband (6400–7500 Å) enables us to measure the gas density via the S ii doublets, in contrast to earlier near-IR studies. Since the fast O iii outflow happens only around rapidly growing central black holes, this object is suitable for investigating the black hole–galaxy coevolution. The obtained data cube exhibits a blue tail in the S ii emission at many lenslets. By fitting the spectrum with the high excess flux at the S ii bluetail, we find a fast (∼860 km s−1), dense (>3000 cm−3), wide-angle, and offset outflow in central 100 pc scales. Although the large opening angle and the high gas outflow-to-accretion ratio may favor the feedback hypothesis, the inferred kinetic power injection rate of this ionized gas outflow seems insufficient to influence the whole host galaxy. A conventional assumption of a low density must have overestimated the feedback process.
By using the Integral Field Spectroscopy mode of the Kyoto Tri-dimensional Spectrograph II we have mapped the two-dimensional distribution of kinematics in a wide variety of emission lines in the ...narrow-line region of NGC 4151. We decomposed the emission lines and defined two components: a narrow component and a broad component. The narrow component has smaller FWHM values, and is spatially more extended than the broad component. We applied a simple model to each component, a rotation in the galactic plane for the narrow component and a biconical outflow model for the broad one. The two-dimensional velocity distributions of the narrow component was well-fitted to a normal rotation in the galactic plane, with the best-fit parameters being similar among the emission lines. We found that the residual maps show similar large positive values at a knot around 6
$^{\prime\prime}$
southwest form the nucleus. For the central region, excluding the knot, the velocity field was fitted better, and the residual was small as the relative wavelength-calibration accuracy of the instrument among lenslets. We modeled the broad component with a simple biconical outflow axisymmetrical with respect to its axis by assuming a constant outflowing velocity, a constant FWHM value, and the emission line strength declining according to a power law with the distance from the nucleus. The best-fit model suggests that PA for the axis of the biconical outflow is close to the direction of the O III line emission elongation. Our line of sight was included within the outflowing bicone, which had filled cones.
Abstract
We find multiple Mg
ii
absorption systems at redshift
z
= 1.66, 2.069, and 2.097 in the spatially resolved spectra of the quadruply gravitationally lensed quasar H1413+1143 utilizing the ...Kyoto tridimensional spectrograph
ii
(Kyoto 3D
ii
) spectrograph on board the Subaru telescope. Here we present the first measurement of differences in Mg
ii
absorption strength of the multiple intervening absorbers, which include ones identified as damped Ly
α
(DLA) absorption systems. Our detection of the significant Mg
ii
absorptions in the spatially resolved spectra reveals the inhomogeneous chemical enrichment on scales of about 12 kpc within the separation of the four sight lines. For the DLA system at
z
= 1.66, the rest equivalent widths (EWs) of the Mg
ii
absorption lines between the four spatially resolved lines of sight change by factors of up to ∼6, which trace the variations in the H
i
absorption strength. This suggests that inhomogeneous cold absorbers that give rise to the strong H
i
/Mg
ii
absorptions dwell on a scale of about 6–12 kpc between the four lines of sight. We also investigate the degree of variation in the EW of the absorption lines between the lines of sight. We find that the systems giving rise to strong absorptions in the spectra of the quadruply lensed quasars tend to have a high degree of variation in absorption strength between the lines of sight toward the lensed quasars.
Abstract
We present the H
α
intensity map of the host galaxy of the repeating fast radio burst FRB 121102 at a redshift of
z
= 0.193 obtained with the AO-assisted Kyoto 3DII optical integral-field ...unit mounted on the 8.2 m Subaru Telescope. We detected a compact H
α
-emitting (i.e., star-forming) region in the galaxy, which has a much smaller angular size (
(1.9 kpc) at full width at half maximum (FWHM)) than the extended stellar continuum emission region determined by the Gemini/GMOS
-band image (
(4.6 kpc) at FWHM with ellipticity
). The spatial offset between the centroid of the H
α
emission region and the position of the radio bursts is
(0.26 ± 0.07 kpc), indicating that FRB 121102 is located within the star-forming region. This close spatial association of FRB 121102 with the star-forming region is consistent with expectations from young pulsar/magnetar models for FRB 121102, and it also suggests that the observed H
α
emission region can make a major dispersion measure (DM) contribution to the host galaxy DM component of FRB 121102. Nevertheless, the largest possible value of the DM contribution from the H
α
emission region inferred from our observations still requires a significant amount of ionized baryons in intergalactic medium (IGM; the so-called “missing” baryons) as the DM source of FRB 121102, and we obtain a 90% confidence level lower limit on the cosmic baryon density in the IGM in the low-redshift universe as
.
We present the H intensity map of the host galaxy of the repeating fast radio burst FRB 121102 at a redshift of z = 0.193 obtained with the AO-assisted Kyoto 3DII optical integral-field unit mounted ...on the 8.2 m Subaru Telescope. We detected a compact H -emitting (i.e., star-forming) region in the galaxy, which has a much smaller angular size ( (1.9 kpc) at full width at half maximum (FWHM)) than the extended stellar continuum emission region determined by the Gemini/GMOS -band image ( (4.6 kpc) at FWHM with ellipticity ). The spatial offset between the centroid of the H emission region and the position of the radio bursts is (0.26 0.07 kpc), indicating that FRB 121102 is located within the star-forming region. This close spatial association of FRB 121102 with the star-forming region is consistent with expectations from young pulsar/magnetar models for FRB 121102, and it also suggests that the observed H emission region can make a major dispersion measure (DM) contribution to the host galaxy DM component of FRB 121102. Nevertheless, the largest possible value of the DM contribution from the H emission region inferred from our observations still requires a significant amount of ionized baryons in intergalactic medium (IGM; the so-called "missing" baryons) as the DM source of FRB 121102, and we obtain a 90% confidence level lower limit on the cosmic baryon density in the IGM in the low-redshift universe as .
We have performed two-dimensional spectroscopy of three nearby E+A (post-starburst) galaxies with the Kyoto tridimensional spectrograph II (Kyoto3DII) integral field spectrograph. In all the cases, ...Hδ absorption is stronger at the centre of the galaxies, but significantly extended at the scale of a few kiloparsec. For one galaxy (J1656), we found a close companion galaxy at the same redshift. The galaxy turned out to be a star-forming galaxy with a strong emission in Hγ. For the other two galaxies, we have found that the central post-starburst regions possibly extend toward the direction of the tidal tails. Our results are consistent with the merger/interaction origin of E+A galaxies, where the infalling-gas possibly caused by galaxy–galaxy merging creates a central starburst, succeeded by a post-starburst (E+A) phase once the gas is depleted.
PDF
