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NGC 5775: Anatomy of a Disk-Halo Interface

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NGC 5775: Anatomy of a Disk-Halo Interface A&A 377, 759–777 (2001) Astronomy DOI: 10.1051/0004-6361:20011046 & c ESO 2001 Astrophysics NGC 5775: Anatomy of a disk-halo interface S.-W. Lee1,J.A.Irwin2, R.-J. Dettmar3, C. T. Cunningham4,G.Golla3,?, and Q. D. Wang5 1 Astronomy Department, University of Toronto, 60 St. George Street, Toronto, Ontario, Canada M5S 3H8 2 Department of Physics, Queen’s University, Kingston, Ontario, Canada K7L 3N6 e-mail: [email protected] 3 Astronomisches Institut der Ruhr-Universit¨at Bochum, Universit¨atsstr. 150/NA 7, 44780 Bochum, Germany e-mail: [email protected] 4 National Research Council of Canada, Herzberg Institute of Astrophysics, 5071 West Saanich Road, Victoria, BC, Canada V9E 2E7 e-mail: [email protected] 5 Department of Astronomy, University of Massachusetts, B-524 Lederle Graduate Research Tower, Amherst, MA, 01003, USA e-mail: [email protected] Received 10 October 2000 / Accepted 12 July 2001 Abstract. We present the first high-resolution study of the disk-halo interface in an edge-on galaxy (NGC 5775) in which every component of the interstellar medium is represented and resolved (though not all to the same resolution). New single-dish CO J =2−1andCOJ =1−0 data, ROSAT X-ray data, and HIRES IRAS data are presented along with HI data which emphasizes the high latitude features. In conjunction with previously published radio continuum (6 and 20 cm) and Hα data, we find spatial correlations between various ISM components in that all components of the ISM are present in the disk-halo features (except for CO for which there is insufficient spatial coverage). The HI features extend to ∼7 kpc above the plane, form loops in position-position space, in one case, form a loop in position-velocity space, and are also observed over a large velocity range. This implies that the disk-halo features represent expanding supershells. However, the shells may be incomplete and partially open- topped, suggesting that we are observing the breakup of the supershells as they traverse the disk-halo interface. There is some evidence for acceleration with z and both redshifted and blueshifted velocities are present, although the gas which is lagging with respect to galactic rotation dominates. The radio continuum spectral index is flatter around the shell rims and we show that this cannot be due to a contribution from thermal gas but rather is due to intrinsic flattening of the non-thermal spectral index, suggesting that shocks may be important in these regions. The Hα emission is located interior to the HI. For feature F3, the Hα emission forms the interior “skin” of the HI shell, yet there appears to be a minimum of in-disk star formation immediately below the feature. We present a picture of a “typical” HI supershell which accelerates and breaks up through the disk-halo interface. Such a feature is likely internally generated via an energetic event in the disk. Key words. ISM: bubbles – ISM: general – ISM: structure – galaxies: general – galaxies: individual: NGC 5775 – galaxies: spiral 1. Introduction present in our own Milky Way. Such observations require high resolution and good signal-to-noise (S/N). Studies of external edge-on galaxies provide an excellent bird’s eye view of galaxy halos and the disk-halo interface without the confusion or distance ambiguities which are When a variety of galaxies is considered, disk-halo ac- Send offprint requests to: S.-W. Lee, tivity has been observed in all components of the interstel- e-mail: [email protected] lar medium (ISM), including molecular gas traced by CO ? Present address: Gesellschaft f¨ur Unix- und (e.g., Irwin & Sofue 1996), dust as observed in the infra- Netzwerkadministration, R¨aterstr. 26, 85551 Kirchheim, red (e.g. Koo et al. 1991) and optical (e.g., Howk & Savage Germany 1999), neutral hydrogen (e.g., Irwin & Seaquist 1990), Hα e-mail: [email protected] emitting 104 K ionized gas (e.g., Pildis et al. 1994), the Article published by EDP Sciences and available at http://www.aanda.org or http://dx.doi.org/10.1051/0004-6361:20011046 760 S.-W. Lee et al.: NGC 5775: Anatomy of a disk-halo interface radio continuum emitting cosmic ray component (e.g., 2. Observations and data reduction Hummel et al. 1991) and the X-ray emitting hot coro- nal gas (e.g., Bregman & Pildis 1994; Wang et al. 1995; 2.1. Radio continuum Dahlem et al. 1996) – as well as many other examples. The radio continuum observations are taken from Duric However, little has been done in the way of systematic et al. (1998) and were obtained with the Very Large multiwavelength studies to see how the components re- Array (VLA) over several years at both 6 and 20 cm late to each other, to discrete star forming regions in the wavelengths in several configurations of the array. disk, and to the global properties of the galaxy. To this Selected images, which have been cleaned and self- end, we have undertaken a multi-wavelength study of the calibrated, are shown in Figs. 1 and 2, i.e., a 20 cm edge-on, IR-bright galaxy, NGC 5775, and present here B + C + D Array 20 cm image at 2300 resolution (Fig. 1b), the first comparative study of the disk-halo interface in a 6 cm C + D array image at 1500 resolution (Fig. 2a), a another galaxy in which every component of the interstel- 20 cm B + C + D array image at 1500 resolution (Fig. 2b) lar medium is represented. and a 20 cm B array image at 500 resolution (Fig. 2d). The −1 −1 NGC 5775 (D =24.8Mpc,H0 =75kms Mpc ) ◦ spectral index map made from the 6 and 20 cm maps at is an edge-on (i =86) galaxy with a high star forma- 1500 resolution is also presented in Fig. 2c. The rms noise × 10 tion rate (LFIR =2.6 10 L ). An optical image of levels are indicated in the figure caption. the galaxy is shown in Fig. 1a. NGC 5775 is interact- ing with its more face-on companion, NGC 5774, 4.03to the north-west (NW) from which it appears to be receiv- 2.2. Neutral hydrogen ing a supply of HI (Irwin 1994), and possibly also with 0 Neutral hydrogen data are taken from Irwin (1994) and a smaller galaxy, IC 1070, 3.9 to the south-west (SW). were obtained using the VLA in its B/C configuration Duric et al. (1998) have modeled the global radio con- with a velocity resolution of 41.7 km s−1.Two(Right tinuum halo of NGC 5775 in terms of two components: Ascension – Declination – Velocity) cubes were made, rep- a broad scale steep spectrum halo with 1/e scale height resenting naturally and uniformly weighted data, with re- of 3.5 kpc, and a smaller flatter spectrum component of sulting rms noise per channel of 0.4 and 0.5 mJy beam−1, ∼1 kpc. Dettmar (1992) made a preliminary comparison respectively. The integrated intensity (zeroth moment) of the Hα and radio continuum emission in NGC 5775 maps made from these data are presented in Fig. 1c (nat- and pointed out the spatial coincidence of the Hα fila- ural weight) and Fig. 1d (uniform weight). The most ob- mentary features and the radio continuum spurs. Collins vious HI extensions are labelled F1 to F3 in Fig. 1d. et al. (2000) found the diffuse ionized gas (DIG) layer in NGC 5775 to have a scale height of 800–900 pc in re- gions away from any obvious discrete high-z features. They 2.3. Far infra-red (FIR) made a comparison of their Hα images with both the radio continuum and total intensity HI, finding a good general Four HI-RES infra-red images (at 12, 25, 60 and 100 µm) correlation in the high-z features in all three components. were obtained by request to the Infra-red Processing and More recently, an optical emission line study by Rand Analysis Center (IPAC). The HI-RES images were ob- (2000) shows a rise in the [OIII]/Hα line ratio with z, tained from the Infra-Red Astronomical Satellite (IRAS) indicating that photoionization at a single temperature observations using the Maximum Correlation Method as cannot alone be producing the emission; shocks and/or described in Aumann et al. (1990). This algorithm makes a change in temperature is required. A decrease in rota- use of the fact that the spatial separation between flux tional velocity with z is also observed, with the highest measurements (“footprints”) is typically less than the full latitude gas showing essentially no rotation. width half maximum (FWHM) of any individual detector, In this paper, we present new CO J =1−0and i.e. the sources have been oversampled. The reconstructed CO J =2−1 observations, new HIRES infra-red images, beam FWHMs constitute improvements by factors of 3.8, and a new X-ray image of NGC 5775. We also present new 3.7, 3.5, and 2.6 over the mean FWHMs of the individual results on the HI distribution using the same data as in detectors for the 12, 25, 60, and 100 µm bands, respec- Irwin (1994) but dealing more specifically with the high tively. The HI-RES maps, the result of 20 iterations of latitude gas. In addition, we present an overview of pre- the algorithm, are shown in Figs. 3a to d. vious results from other wavebands, highlighting features which may be related to the interaction, the in-disk dis- 2.4. Hα tribution, and the high latitude and halo emission.
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