Shin’ichi Tamura

HaTr 10, a Planetary Nebula with Extremely Strong Nitrogen Lines

ABSTRACT Optical spectra and direct images reveal that a very faint, scarcely studied object (HaTr 10) which appears as an incomplete elliptical ring of 0 \documentclass{aastex} \usepackage{amsbsy} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{bm} \usepackage{mathrsfs} \usepackage{pifont} \usepackage{stmaryrd} \usepackage{textcomp} \usepackage{portland,xspace} \usepackage{amsmath,amsxtra} \usepackage[OT2,OT1]{fontenc} \newcommand\cyr{ \renewcommand\rmdefault{wncyr} \renewcommand\sfdefault{wncyss} \renewcommand\encodingdefault{OT2} \normalfont \selectfont} \DeclareTextFontCommand{\textcyr}{\cyr} \pagestyle{empty} \DeclareMathSizes{10}{9}{7}{6} \begin{document} \landscape

Analysis of Internal Motions in the Halo Planetary Nebula H4-1

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G247.8+4.9: A Newly Discovered Optical Supernova Remnant in Puppis

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Highly Resolved Spectroscopic Study of PNe with HIDES A Case Study of NGC 6572

ABSTRACT Up to now, 10 planetary nebulae have been regarded as halo planetary nebulae (halo PNe). We obtained low‐ and moderate‐dispersion spectra of the spatially resolved halo planetary nebula H4‐1 in the wavelength region of 3700–6800 A with the Cassegrain Spectrograph of the 74 inch telescope. At moderate dispersions, we were able to observe [O iii] λλ4959, 5007 and Hα of H4‐1 at several position angles (P.A.). We assumed that the widths of these emission‐line profiles were due to Doppler broadening and that these emission lines were composed of several Gaussian components. Multiple Gaussian deconvolution analysis of such emission lines indicated H4‐1 has broad wing components (∼600 km s−1) at P.A. 135° and 180°. We think H4‐1 has a “bipolar flow” between P.A. 135° and 180°. From low‐dispersion spectra, we confirm that H4‐1 is a metal‐poor PN. In spite of the lack of spatially resolved images at present, we believe that H4‐1 has a bipolar flow and that its axis is almost parallel to the line of sight,...

Spectroscopic Diagnosis on Symbiotic Star Z and During Recent Outburst Phase

As a first step to investigate a newly detected possible supernova remnant in Puppis, a few optical spectra have been obtained. The spectra of this extremely faint nebula, although of poor quality, show strong (N ii) 6583/6548 A u emission. Radial velocities derived from the (N ii) 6583 A u line amount to 50 km s 1 , for both the easternmost and westernmost optical borders of the nebula, and a distinctly blueshifted velocity relative to this value for an emission region close to the eastern rim. In order to check whether the remnant might be akin to the nebula W50 associated with the compact source SS 433, a spectrum of four stars near the center of the image of the nebula was taken; it showed them to be of quite ordinary type and exhibits some traces of (nebular) (N ii) 6583 A u emission. No IRAS source is located at or within the boundaries of the nebula, which coincides with an extended radio source of about 78 mJy at 4850 MHz. The star that gave rise to the remnant may have been a remote member of the Pup OB2 association, at a distance of about 5 kpc.

Symbiotic Stars with Highly Resolved Emission Line Profiles

We have analyzed the internal kinematics of the point‐symmetric, young (1,100 yr) planetary nebula (PN), NGC 6572 using high‐resolution (λ/Δλ = 50,000 and 61,000) optical long‐slit spectra at six position angles including [O III]λ5007, Hα, and [N II]λ6583 obtained with HIDES (HIgh Dispersion Echelle Spectrograph) combined with the f/29 coude focus of the 74‐inch telescope at the Okayama Astrophysical Observatory (OAO, National Astronomical Observatory, Japan). Examination of these emission lines led to our discovery of a collimated outflow. This outflow has a different expansion velocity and direction from that of the main nebular shell. We also examined the physical conditions of the collimated outflow. The excitation mechanism and the behavior of Te and Ne are consistent with those found in the collimated components of other point‐symmetric PNe.

Expansion Analyses on Planetary Nebulae

This report aims to present preliminary results of spectroscopic diagnosis on symbiotic star Z And during recent outburst phenomenon. We have made high dispersion spectroscopy with HIDES (HIgh Dispersion Echelle Spectrograph) at Okayama Astrophysical Observatory (OAO) since Jan. 2001. Z And is a binary system with an orbital period of 758.8 day. We are concerned with distinguishing spectroscopic characteristics at outburst phase from quiescent one, and from the orbital change. The most conspicuous feature of spectroscopic results is the violet shift of He IIλ686 and [Fe VII] λ6087 as a whole and susequent gradual returning to their original wavelengths. Broad Hα line-profiles do not show drastic changes except complicated behavior of violet side those are already noticed by previous study.

High Velocity Collimated Flow in a Halo Planetary Nebula, H 4-1

This report is concerned with spectroscopic diagnoses on the gaseous region of symbiotic stars based upon our recent work(Ikeda and Tamura, 1999: submitted to P.A.S.Japan). It is now widely accepted that the symbiotic star is a binary system which consists of a cool giant and a hot dwarf surrounded or accompanied with the ionized gas, probably together with dusts. Usually we can not recognize a hot star in the spectrum directly. Therefore, it looks like that a cool giant coexist with the ionized gas which produce rich emission-lines. This is the origin of the designation as symbiotic stars.

Four New Evolved Planetary Nebulae

Since planetary nebulae(PNe) are defined as the expanding ionized gas surrounding hot central stars, the most important and fundamental subject is to study expansion characteristics. What and how can we determine a typical expansion velocity of individual nebula? In spite of great success of Perek and Kohoutek Catalog(1967) and a recent Strasbourg-ESO Catalogue(992), PNe researchers have suffered from the lack of sufficiently large samples of expansion measurements on various type of PNe.

Expansion Velocities of [NII] and [OIII] from Compact Planetary Nebulae

H 4-1, PNG 049.3+88.1 (α = 12h59m27.6s, δ = +27°38′14″, 2000), was one of well known halo Planetary Nebulae (PNe). During our program to study the expanding characteristics of PNe, the long-slit spectroscopic observations were made by the cassegrain spectrograph of the 74 inch telescope at the Okay ama Astrophysical Observatory in March 1995.