Äîêóìåíò âçÿò èç êýøà ïîèñêîâîé ìàøèíû. Àäðåñ îðèãèíàëüíîãî äîêóìåíòà : http://www.naic.edu/~tghosh/a1908/thesis1-final.pdf Äàòà èçìåíåíèÿ: Sat May 12 01:45:01 2007 Äàòà èíäåêñèðîâàíèÿ: Sun Apr 10 17:13:16 2016 Êîäèðîâêà: Ïîèñêîâûå ñëîâà: m 106

HI 21-cm and OH 18-cm Arecib o Observations of Galaxies with High Infrared Luminosity from the 2 Jy IRAS-NVSS Sample
Mar´ Ximena Fern´ ia andez

Advisors: Dr. Emmanuel Momjian Tapasi Ghosh Christopher Salter

Dr. Dr.

(NAIC-Arecibo Observatory) Professor Debra Elmegreen (Vassar College)

Vassar College Department of Physics and Astronomy Spring 2007

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Abstract
HI 21-cm and OH 18-cm spectral line measurements are presented for 85 infrared galaxies from the 2 Jy IRAS-NVSS sample observed with the 305-m Arecibo Radio Telescope. We detected HI in 82 galaxies (18 new detections), and OH in 7 galaxies (4 new detections). In some cases, the HI spectra show the classic double-horned or single-peaked emission profiles.However, the ma jority exhibit distorted features indicating that the galaxies are in interacting and/or merging systems. From the HI and OH observations, important properties from the galaxies are derived, which are then used to look for correlations in the sample. The radio-FIR correlation is confirmed, and there are some potential correlations between the HI mass and other properties. The ULIRG IRAS 23327+2913 is discussed in greater detail since both its HI emission and OH megamaser activity are new detections. This ULIRG consists of two galaxies separated by 0.2 arcmin and it is thought to be an early-stage merger.

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Contents

I. Intro duction A. Neutral Hydrogen B. OH Megamasers and Absorption C. The Present Study I I. Observations and Data Reduction A. Sample Selection B. Observations C. Data Reduction D. HI Detections 1. Emission and Non-Detections 2. Absorption E. OH Observations 1. OH Megamasers 2. OH Absorption 3. OH Non-detections I I I. Discussion A. Special Ob jects 1. IRAS 21054+2314 2. IRAS 22523+3156 3. IRAS 23327+2913 B. Statistical Analysis C. Correlations 1. Radio-FIR Correlation 2. HI Mass Correlations 3. Other Correlations IV. Conclusion V. References

4 6 7 8 8 8 9 10 10 10 12 13 13 14 14 15 15 15 15 16 16 17 18 18 18 19 46

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I.

INTRODUCTION

In the 1980's, the Infrared Astronomical Satel lite (IRAS) discovered a myriad of previously undetected ob jects, most of whose radiation is being emitted at infrared wavelengths (Houck et al. 1984, 1985; Soifer et al. 1984, 1986; Rieke & Lebofsky 1986). The IRAS mission was launched in 1983 and conducted the first all-sky survey at far-infrared wavelengths. This unbiased, sensitive survey at 12, 25, 60, and 100 µm, increased the number of catalogued ob jects by 70%, detecting about 350,000 new sources. Some of the most important IRAS observations include the following: a disk of dust grains around the star Vega, six new comets, infrared cirrus (wisps of warm dust) which could be found in almost every direction of space, the core of the Milky Way, and thousands of galaxies with very strong infrared emission. At bolometric luminosities above 1011 L , these infrared galaxies become the dominant population of extragalactic ob jects in the local universe (z 0.3). These galaxies are subdivided into three categories: luminous (LIRGs, Lir > 1011 L ), ultraluminous (ULIRGs, Lir > 1012 L ), and hyperluminous (HyLIRGs, Lir > 1013 L ; Sanders & Mirabel 1996). Even though these galaxies are relatively rare, some studies suggest that the ma jority of galaxies with LB > 1011 L 1987). Luminous infrared galaxies tend to be in strongly interacting/merging systems of molecular gas-rich spirals. 1011 < L At L
ir

go through a stage of intense infrared emission (Soifer et al.

< 1011 L , most IRAS galaxies are single, gas-rich spi-

rals whose infrared luminosity can be accounted for by star formation. Over the range
IR

< 1012 L , most of the galaxies are in interacting/merging systems that have

enormous quantities of molecular gas. At the lower end of this range, the bulk of the infrared luminosity is due to warm dust grains heated by a nuclear starburst, while active galactic nuclei (AGN) become increasingly important at higher luminosities. Galaxies with Lir > 1012 L are believed to be advanced mergers powered by a combination of starburst and AGN (Sanders & Mirabel 1996). Most luminous infrared galaxies are characterized by their dense gas concentrations, having as much as 1010 M of gas within the merger nucleus (0.5 kpc). It is therefore

important to study these regions to comprehend the evolutionary stages of many ob jects in the universe. The study of infrared galaxies provides a better understanding of the galactic

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merger environment in which a significant fraction of the stars in the universe likely formed. Furthermore, ULIRGs are believed to represent an evolutionary stage in the formation of active galaxies and elliptical galaxies (Sanders et al. 1988). Interacting systems play an important role in the metal enrichment of the intergalactic medium (IGM). There are optical and X-ray data that indicate the presence of superwinds in galaxies with high infrared luminosities. Such winds can be explained by the kinetic energy from supernovae and winds from massive stars in a starburst galaxy driving a largescale outflow that can shock, heat and accelerate the circumnuclear gas. Heckman (1990) concludes that the amount of material ejected by such a wind from a galaxy is enormous, thus having a significant role in enriching the environment. Previous studies have shown that many ULIRGs have K-band profiles that are well fit by an r
- 1/4

law, as is usually valid for elliptical galaxies (Stanford & Bushouse 1991, Kim 1995).

Even though there is strong evidence indicating that the mergers of spirals form ellipticals, there are two properties that need to be addressed: the abundance of globular clusters in the extended halos of ellipticals, and the low content of gas in ellipticals which leads to the question of what happened to the abundance of gas present in interacting systems. The first property could be explained by HST observations of star clusters found in merging systems which may evolve into globular clusters (Whitmore et al 1993, Meurer et al 1995). This suggests that the number of globular clusters increases during the merger of gas-rich spirals. In regards to the second property, it has been hypothesized that the collisions between massive gas-rich spirals might trigger the formation of dwarf galaxies in the neighborhood, which would account for all of the gas originally present in merging systems (Zwicky 1956, Mirabel et al.1991). An optical study carried out by Sanders et al. (1988) of a sample of ultraluminous infrared galaxies resulted in a model that explains the connection between ULIRGs and quasars. The model assumes a merger of two late-type spiral galaxies as the optimum interaction for producing maximum nuclear luminosity. Once the inner disks of the galaxies overlap, frequent molecular cloud collisions will start to occur, which increases the star formation rate. These collisions will dissipate orbital angular momentum, resulting in a decreased orbit radius and the funneling of gas into the merger nucleus. The increased star formation rate and the concentration of molecular clouds to the merger nucleus will result in the appearance of a nuclear starburst before the two galaxies merge. Once they merge, the molecular gas 5


will be densely concentrated within a radius of < 1 kpc. At this stage, a self-gravitating disk may be formed, this becoming an important mechanism for further dissipation of angular momentum and efficiently fueling an AGN which contributes significantly to the observed far-infrared luminosity. The authors of this study conclude that all ULIRGs develop into quasars and a substantial fraction of quasars seem to develop from ULIRGs.

A.

Neutral Hydrogen

A neutral hydrogen atom consists of an electron orbiting a single proton. The proton and electron spin orientations are either parallel or antiparallel. The atom is in an excited state when the spins are aligned in the same parallel direction. When the electron spontaneously changes spin from parallel to antiparallel, a photon is emitted at a frequency of 1420.40575 MHz (21-cm wavelength). This process is known as the hyperfine transition of the hydrogen atom. Even though this is considered to be a forbidden transition due to the unlikely probability of it occurring, it is easily observed with radio telescopes because of the abundance of neutral hydrogen in the universe. Neutral hydrogen is found in most disk galaxies, and is the fundamental element in the star formation processes. HI clouds provide the starting point for the collapse of matter into stars. When there is a high surface density of neutral hydrogen in a galaxy, it means that there are active star formation processes. A lack of it would indicate a barren galaxy with an aging star population (Giovanelli & Haynes, 1988). Since its discovery in 1951, the HI line has become an important tool for studying the structure and dynamics of galaxies both because it is easily detected, and relatively easy to interpret. Previous HI observations of ULIRGs have revealed very broad absorption lines indicating rotation plus large amounts of turbulent gas (Mirabel 1982). VLA observations show that these galaxies have the absorbing HI situated in the inner few hundred parsecs in front of the radio continuum sources (Baan et al. 1987). Most of the HI seen in absorption is infalling toward the central source (Martin et al 1991).

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B.

OH Megamasers and Absorption

MASER (Microwave Amplification by Stimulated Emission of Radiation) activity amplifies emission lines at specific wavelengths. The first step in this process is known as population inversion, where electrons in molecules are pumped to a higher energy level. Then, a photon of the right frequency causes the electron to jump to a lower energy level, emitting energy and stimulating neighboring molecules to do the same. This kind of non-thermal radiation causes an amplification of weak individual line emission creating a coherent maser line. Masing occurs naturally in dense molecular regions. In the Milky Way, cosmic maser emission occurs in the immediate neighborhood of young stellar ob jects or in circumstellar envelopes around evolved stars (Lo, 2005). Extragalactic megamasers are typically more than a million times the luminosity of Galactic masers, and are therefore called megamasers. OH megamaser activity occurs in the central regions of some of the most luminous infrared galaxies. There have to be three conditions for an OH megamaser (OHM) to occur: high molecular density to have an optical depth of 1, a pumping mechanism to invert the OH molecules in the ground state, and a source with a wavelength of 18 cm to stimulate maser emission (Burdyuzha & Komberg, 1990). These three conditions are found in the galactic merger environments of the most luminous far-infrared (FIR) galaxies. Galaxy interactions cause high concentrations of gas near the merging nuclei, creating strong FIR dust emission from reprocessed starburst light and AGN activity, and producing radio continuum emission. Studying OHMs is important because they could be used as tracers of galaxy mergers, dustobscured starburst nuclei, and formation of binary supermassive black holes (Darling & Giovanelli 2000, 2001, 2002). Studies of the extragalactic OH 18-cm lines began in the 1970's with the first detection of OH absorption in NGC 253 and M 82 (Weliachew, 1971). Since then, several surveys have been carried out by telescopes of large collecting area looking for OH megamasers and absorbers. Baan (1989) conducted a study to identify the differences between the galaxies that exhibit OH emission and those with absorption. He concluded that the emission usually occurs in galaxies with higher FIR luminosities and flatter 100-25 µm spectra than the ones with absorption features. Darling & Giovanelli (2000) undertook a ma jor survey with the upgraded Arecibo telescope, detecting 50 new OH megamasers, and doubling the number of known OHMs.

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C.

The Present Study

The present study analyzes the HI 21-cm and OH 18-cm spectra of a sample of 85 galaxies with high infrared luminosities, including classically defined LIRGs and ULIRGs. Since the ultimate source for starburst and AGN activity is the interstellar medium, it is essential to study the atomic and molecular transitions in order to gain a better understanding of the gas present in these ob jects. One of the principal goals of this study is to determine properties from the HI and OH spectra in order to compare sources containing AGNs and those with pure starbursts through their velocity widths and the derived mass values. Another goal is to study galactic evolution out to z=0.2. The most interesting ob jects in this sample can be followed-up with VLA and VLBI observations to study gas dynamics on both large and small angular scales. This study is important because it involves various galaxies that have not been included in previous surveys because of narrower selection criteria and instrumental limitations. Our sample also includes 64 galaxies that have been previously detected, so that we can both provide improved spectra and carry out variability studies on a time scale of 15-20 years. Below, we adopt the currently preferred cosmology of H0 = 71 km s-1 Mpc-1 ,
M

= 0.27,

and = 0.73 (Spergel et al. 2003). Using this cosmology gives more accurate luminosity distances, but does not allow the classification of galaxies as LIRG or ULIRG using existing definitions, since these definitions were set for a different cosmology.

I I.

OBSERVATIONS AND DATA REDUCTION A. Sample Selection

The galaxies studied in this thesis are a first set of ob jects extracted from the 2 Jy IRASNVSS sample (Yun et al., 2001). The 2 Jy IRAS-NVSS sample has 1809 IRAS sources whose 60 µm infrared flux densities are greater than 2 Jy, with 1.4-GHz radio counterparts from the NRAO-VLA Sky Survey (NVSS; Condon et al. 1998). From the 2 Jy IRAS-NVSS survey, galaxies that met the following three criteria were selected for the present study: (1) they lie within the Arecibo Sky (i.e. -1 < declination < 38 ), (2) have far-infrared luminosities of at least 109 L , and (3) have heliocentric velocities between 0 and 50,000 km s-1 . The resulting number of galaxies that meet these criteria is 582. The present study 8


includes 85 of these galaxies whose right ascensions lie in the range 20h-00h. Table 1 describes the sample in the following format. Column (1) lists the IRAS name. Column (2) and (3) are the coordinates of the galaxy (epoch J2000). Column (4) lists the optical redshift retrieved from the NASA/IPAC Extragalactic Database (NED). Column (5) is the 60µm flux density from the IRAS Faint Source Catalogue (FSC), where available. If not, this is indicated by an asterisk, and the Point Source Catalogue (PSC) value is given instead. Column (6) is the 1.4-GHz flux density from the NVSS survey. Column (7) is the morphology listed in NED and in the Hyperleda database (Paturel et al. 2003). Columns (8) and (9) are the inclination and logD25 (where, D25 is the ma jor axis of the 25th magnitude isophotal ellipse) respectively, which were retrieved from Hyperleda. The values for lodD25 are in units of log (0.1 arcmin).

B.

Observations

The 85 galaxies were observed with the 305-m Arecibo radio telescope between July and November 2004 using the L-wide receiver. The receiver's frequency cut-off at the low end is 1100 MHz, which is well below the sample limit of 50,000 km s-1 . The four boards of the Arecibo Interim Correlator were utilized to simultaneously observe the following redshifted transitions: HI 21-cm line (1420.40575 MHz), OH 18-cm main lines (1665.4018 and 1667.359 MHz), and OH 18-cm satellite lines (1612.231 and 1720.053 MHz). A bandwidth of 12.5 MHz was used for each interim correlator board, centered at the frequency of the redshifted transition, with 1024 spectral channels per polarization. We utilized the total-power position switching (ON-OFF) observational mode for all ob jects with flux densities lower than 75 mJy at 1.4 MHz. Double Position Switching (DPS) was used to observe ob jects with higher radio flux densities in order to minimize baseline ripples.

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C.

Data Reduction

The data were reduced with AO IDL standard routines and some special purpose codes developed by the AO staff. The spectra of the sources observed with the ON-OFF mode were converted to a flux in Janskys using the noise cal and the standard gain curves. For the sources observed in DPS mode, bandpass calibration sources were needed to convert the ratio spectra to Janskys. Hanning smoothing was applied to the raw spectra. For each spectra, the two polarizations were added to improve the signal-to-noise ratio by 2, and then smoothed by 9 channels. The baseline for each averaged spectrum was fit by a polynomial and subtracted.

D.

HI Detections

We detected HI in 82 of the 85 galaxies in both emission and absorption; 18 of these had not been previously reported in the literature. IRAS 21396+3623, one of the three non-detections, was observed at a wrong redshift since this was incorrectly listed in the 2-Jy IRAS NVSS Sample. This source will not be included in our analysis. The sources observed in DPS mode will be indicated by a in the HI tables.

1.

Emission and Non-Detections

Some of the HI emission profiles showed single peak or double horn distributions, both characteristic of non-interacting galaxies. However, as expected, a ma jority of the galaxies observed had distorted spectra indicating that they are in interacting/merging systems. The galaxies in interacting systems had higher infrared luminosities than the non-interacting spirals. Figure 1 and Figure 2 present the HI emission-only spectra (new and previously detected, respectively). Figure 3 includes the spectra of the two non-detections in our sample.

a. Parameters derived from HI emission spectra Three different schemes were implemented to measure the central velocity of the line emission, the width, and the flux-density integral. Several important properties can be derived from these three numbers. The luminosity distance, DL , is obtained from the observed 10


central velocity with a cosmology calculator, adopting the currently preferred cosmology of H0 = 71 km s
-1

Mpc-1 , M = 0.27, and = 0.73. The far-infrared luminosity is derived

with the following formula: L
FIR 2 = 3.96 x 105 DL (2.58f60 + f100 )

(1)

where DL is in Mpc, and f60 and f100 are the 60 and 100 µm flux densities in Jy from the FSC, if available, or from the PSC. The resulting L
FIR

is in units of L . The total infrared

luminosity is calculated with the following formulae: L and, FIR = 1.8 x 10- where FIR is in units of W m-2 . The mass of hydrogen in solar units is given by:
2 = 2.36 x 105 DL 14 IR 2 = 4 DL FIR

(2)

[13.48f12 + 5.16f25 + 2.58f60 + f100 ]

M where the S dv is in Jy km s
-1

HI

S dv

(3)

and the luminosity distance, DL , is in Mpc.

The dynamic mass for those galaxies with an i > 30 is calculated with the following equation: M
Dyn

= 2.325 x 105 R V

2 rot

(4)

where R is the linear size of the galaxy in kpc, which can be calculated from the logD25 values, and Vrot is the inclination corrected velocity width in km s-1 . The resulting M in units of M
Dyn

is

b. Emission Table Table 2 lists the integration times for the observations, and the parameters derived from the HI spectra for the sources that exhibit emission, plus those that were not detected (which are marked by an asterisk). Some spectra (indicated by ) exhibit both emission and absorption features. For these, the table contains only information from the emission part of the spectra, and the derived flux density integrals are lower limits since some of the emission might be hidden by absorption features. The absorption components will be discussed in the following section. The format of Table 2 is as follows: 11


Columns (1) and (2) are the IRAS name and the total ON-source integration time. Column (3) and (4) are the rms and the signal-to-noise ratio (SNR). Column (5) is the heliocentric velocity at which the HI emission was observed. For non-detections, the velocity from the redshift listed in Table 1 will be listed. Column (6) is the Full Width at Half Maximum (FWHM). Column (7) is the flux density integral of the HI line. In the case of the non-detections, the entered value will be given by 3 x rms noise x 100 km s-1 . Column (8) is the luminosity distance. Column (9) is the far-infrared luminosity calculated with Eq. 1. Column (10) is the total infrared luminosity derived from Eq.2. Column (11) is the total mass of neutral hydrogen given by Eq.3 . Column (12) is the dynamical mass of the galaxy calculated with Eq.4.

2.

Absorption

There were 10 HI spectra that displayed absorption features, 7 of which also had an emission component. Figure 4 has the spectra of those sources with both emission and absorption. Figure 5 contains the spectra of the three galaxies with absorption-only features.

a. Parameters derived from HI absorption spectra Each of the averaged spectrum was converted into fractional absorption to then attain the optical depths using the following equation: Fa =1-e F ( < 0.1), = 1 -
Fa F -

(5)

where Fa /F is the fractional absorption and is the optical depth. For small values of .

The area under the absorption feature ( dv) was obtained by numerical integration of the tau vs velocity plot (optical depth spectrum). From this integral, the column density can be found by using the following formula: N(HI)/Ts = 1.823 x 10
18

dv

(6)

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The resulting column density is given in units of cm-2 K-1 . This equation assumes a "covering factor" of unity.

b. Absorption table Table 3 lists the parameters derived from the absorptions in the following format: Columns (1) and (2) are the IRAS name and the total ON-source integration time. Column (3) and (4) are the rms and the signal-to-noise ratio (SNR). Column (5): heliocentric velocity at the center of the absorption feature. Column (6) is the width of the absorption feature. Column (7): is the peak value of the optical depth. Column (8) is the column density divided by the spin temperature with Equation 5.

E.

OH Observations

There were 7 detections of OH activity: 3 megamasers and 4 absorbers shown in Figure 6 and 7, respectively. Out of these, 1 OHM and 3 absorbers are new detections. There were no detections in the satellite lines.

1.

OH Megamasers

Table 4 contains information about the 3 OHMs in the sample listed in the following format: Columns (1) and (2) are the IRAS name and the total ON-source integration time. Column (3) and (4) are the rms and the signal-to-noise ratio (SNR). Columns (5) and (6) are the peak of the flux density for each of the main lines. Column (7) is the velocity at which the 1667 line was detected. Columns (8) and (9) are the velocity width of the 1667 and 1665 emission lines. Columns (10) and (11) are the integrated flux density for each of the main lines. Column (12) lists the hyperfine ratio, which can be found by dividing Col.10 by Col.9. In thermodynamic equilibrium conditions, this ratio would be RH = 1.8, and it increases as the saturation of masing regions increases.

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Column (13) lists the predicted OH luminosity which can be attained with the following equation (Kandalian 1996): log L
pred OH

= 1.38 log L

FIR

- 14.02

(7)

2.

OH Absorption

Table 5 lists the information about the OH absorbers in the following columns: Columns (1) and (2) are the IRAS name and the total ON-source integration time. Column (3) and (4) are the rms and the signal-to-noise ratio (SNR). Column (5) is the velocity at which the 1667 line was detected. Columns (6) and (7) are the velocity width of the 1667 and 1665 absorption lines. Columns (8) and (9) are the peak values of the optical depths for each of the main lines. Columns (10) and (11) are the integrated optical depths for each of the main lines. Column (12) lists the hyperfine ratio, which is attained by dividing the integrated optical depths. Column (13) is the 1667 hydroxyl column density divided by the excitation temperature. This value can be found by using the following equation: N where
OH

/T

ex

= 2.35 x 1014

dv

(8)

dv is the integrated optical depth of the 1667 MHz absorption feature. The

resulting column density is given in units of cm-2 K-1 .

3.

OH Non-detections

Table 6 lists relevant data for the non-detections in the four OH transitions. There were no detections at the 1612 and 1720 MHz frequencies. The data is organized in the following format: Column (1) and (2) are the IRAS name and the rms for the main lines. Columns (3) and (4) are the predicted and maximum OH luminosity. Both values are derived from the 1667 line. The first value is calculated with Eq. 7 and the maximum OH luminosity is determined with the following equation:

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2 where DL

v o (9) c (1 + z ) is the luminosity distance, is the rms value listed in column 2, v = L
max OH 2 = 4 DL 1.5

150 km s-1 , c is the speed of light, o is the frequency (in this case, 1667 MHz) and z is the redshift. Columns (5) and (6) are the rms values for the 1612 and 1720 transitions.

I I I. A. 1.

DISCUSSION Sp ecial Ob jects IRAS 21054+2314

This galaxy showed HI emission and absorption, and OH absorption. Both of these detections were not previously reported in literature. This LIRG is at a redshift z = 0.049. As seen in the Figure 8, the HI and OH features lie at about the same velocity. The HI spectrum displays the absorption feature to be at a higher velocity than the emission, indicating a possible scenario where there is infalling material towards the central source. The OH spectrum shows absorption at the 1667 MHz line. It would be interesting to use interferometers to map the neutral hydrogen and hydroxyl in this galaxy in order to gain a better understanding of the HI and OH distribution. There is no information about this ob ject in the literature, only the standard optical and photometry information.

2.

IRAS 22523+3156

This ob ject also displays previously unreported HI and OH lines (Figure 9). IRAS 22523+3156 has a relatively low IR luminosity, and is at a redshift of z = 0.021. The HI spectrum shows a peculiar shape, since it has a deep absorption feature in the middle of the emission line. The OH spectrum displays two nicely defined absorption features at rest frequencies of 1665 and 1667 MHz. The hyperfine ratio is 1.3, indicating that the conditions are close to, but not completely in thermodynamic equilibrium. The 1667 MHz line lies at the same velocity as the absorption feature in the HI spectrum, showing that they originate from the same location. This is also an excellent candidate for interferometeric maps and it 15


would give us a better understanding of how the HI and OH is distributed in the galaxy. As in the previously discussed ob ject, there has not been a ma jor study done on this galaxy.

3.

IRAS 23327+2913

IRAS 23327+2913 proved to be the most interesting ob ject in our sample since we detected both HI emission and OH megamasing activity in this galaxy for the first time. This ULIRG is at a redshift z = 0.107. A recent study by Dinh-Vi-Trung et al. (2001) of this ob ject revealed that it is a system of two interacting galaxies separated by 20 kpc. Figure 10 shows contour plots of this galaxy. The northern component of the interacting pair is disturbed, while the southern component is a normal spiral with a very thick bar structure. This ob ject is particularly interesting because it is an ultraluminous galaxy but it is still in the early stages of interaction, contrary to the belief that ULIRGs are advanced mergers. As seen in Figure 10, the HI spectrum displays the presence of the two nuclei, 300 km s
-1

apart and separated by a bridge of material. The bulk of the HI emission seems to

be associated with the southern component while the weaker shoulder corresponds to the northern component. The spectrum of the OH main lines shows a broad double-peaked profile at 1667 MHz, and seems to be associated with the southern component. No emission is detected from the northern, disturbed component of this galaxy. Follow up observations with interferometers are needed to better study and understand the HI and OH emission of this unusual ULIRG.

B.

Statistical Analysis

The following table is a statistical comparison between the studied sample, and the UGC/ LSc sample of Roberts & Haynes (1994) which tend to have lower infrared luminosities since they are non-interacting galaxies. All of the listed numbers are median values.

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Parameter M M
HI

Our Sample 5.1 18.1 0.029 ) 10.63 51.29

UGC 5.62 22.6 0.03 4.64 9.89

LSc 1.41 7.1 0.03 4.45 1.96

Comment Sample is not very different to UGC. Sample is not very different to UGC. Gas fraction is comparable Sample is significantly higher Sample is an order of magnitude higher

(109 M ) (1010 M )
Dyn -2

Dyn

MHI /M
HI

(M pc

LFIR (109 L )

The numbers in the first three rows seem to be comparable. We were expecting to see a bigger difference in the ratio between the HI mass and the dynamical mass, since we thought the amounts of gas relative to the total mass of the galaxy would be different for interacting galaxies. There is, however, a considerable difference in the numbers in the last two rows. The HI surface density is much higher in this sample, which implies a higher star formation rate. As it is seen in the last row, the FIR luminosity is much higher than the UGC/LSc.

C.

Correlations

Various plots were made in order to find correlations between the properties of the galaxy. The following table lists the plot and its respective correlation factor. If the factor is at least 60%, then one can say there is a correlation.
Correlation Radio-FIR Flux Radio-FIR Lum HI Mass-FIR Lum HI Mass-Radio Dyn Mass-HI Mass Dyn Mass-FIR Lum Dyn Mass-Radio Coefficient (%) 70.4 89.6 36.3 42.0 51.5 13.7 17.3

17 1


1.

Radio-FIR Correlation

There has been a well studied correlation between radio and far-infrared properties. Figure 11 shows this correlation. The first plot compares the 1.4 GHz radio and 60µm flux densities, while second one compares the 1.4 GHz and 60µm luminosities. As it can be seen, the second plot shows a stronger correlation and this is because distance is taken into account when dealing with luminosities. As the previous table shows, both plots have correlation coefficients higher than 60%, which demonstrate that this sample does show the famous Radio-FIR correlation.

2.

HI Mass Correlations

There were three plots made in order to examine possible correlations between the mass of neutral hydrogen and other properties. The first plot (Figure 12) shows an extremely weak correlation between the 60µm luminosity and the HI mass. The correlation factor is 36.3 %, indicating there is not a defined relation between these quantities. This correlation would make sense because FIR radiation is related to star formation activity, meaning there is a need for large HI content for higher star formation rate. Figure 13 shows the relation between the HI mass and the 1.4 GHz radio flux density. This is another case for a weak correlation since its correlation factor is 42%. This correlation might imply that most of the 1.4GHz emission is associated with star formation activity, and thus it has a higher value for a highe neutral hydrogen mass. There is a stronger correlation between the HI mass and the dynamic mass (Figure 14). Its correlation factor is 51.5%, indicating there is a more defined relation between these two quantities. This correlation makes sense since this sample mostly consists of spirals. The correlation seen in the plot would only apply to spirals, since galaxies with a low-surface brightness tend to be dominated by dark matter.

3.

Other Correlations

The other two plots relate the dynamic mass with the 60µm luminosity (Figure 15), and the 1.4 GHz radio flux density (Figure 16). As seen in the plots and the low correlation factors, there is no relation between these quantities. 18


IV.

CONCLUSION

This thesis presents the HI 21-cm and OH 18-cm observations of a subset of the 2 Jy IRAS-NVSS sample. Neutral hydrogen was detected in almost all of the observed galaxies (82 out 84), and seven of them had hydroxyl. Out of these, 18 were new HI detections, and 4 OH new detections. There are at least three intriguing ob jects that should be mapped with interferometers to understand their HI and OH distribution. From the HI and OH detections, important properties were derived such as the luminosity distance, infrared properties, the amount of hydrogen present, the dynamic mass of the galaxy, and HI and OH column density. From these properties, various plots were made to look for possible correlations. This sample shows the previously-known Radio-FIR correlation. In addition to this, there were some potential correlations: HI mass-dynamic mass, HI mass-60µm luminosity, and HI mass-1.4GHz radio flux density. These correlations should be further examined once the complete sample is studied. There are various things that can still be done. The most important is to divide this sample between those ob jects that have an AGN, and those that do not. It is important to compare the properties of these two groups in order to determine if there is any significant difference between them. Another important thing to do is to study the previously-known cases of HI and determine if there is variability. Furthermore, it is important to observe the rest of the galaxies in order to make broader conclusions about the 2 Jy IRAS-NVSS sample, which mostly consists of galaxies with high infrared luminosities.

19


ABCD.9""$9E""#$
"7"";

IRAS 20178-0052
0.012

IRAS 20198+0159

0.275
0.011

"7"":

0.270

Flux Density (Jy)

<'=>.?&+5(,0.1@06

Flux Density (Jy)

0.010

0.265

"7""9

0.009

0.260

"7""8
0.008

0.255
"7"""
0.007

0.250
!""" !#"" $""" %&'()*&+,-(*./&')*(,0.123456 $#""

5000

5500 Heliocentric Velocity (km/s)

6000

11500

12000 12500 Heliocentric Velocity (km/s)

13000

IRAS 20332+0805
0.007
0.029

IRAS 20369+0150
0.018

IRAS 20381+0325

0.006

Flux Density (Jy)

Flux Density (Jy)

0.005

0.027

Flux Density (Jy)
3400 3600 3800 4000 4200 Heliocentric Velocity (km/s) 4400 4600

0.028

0.016

0.005

0.014

0.005

0.026 0.012

0.004 7500 8000 Heliocentric Velocity (km/s) 8500

0.025 7500 8000 Heliocentric Velocity (km/s) 8500

0.007

IRAS 22032+0512

IRAS 22388+3359
0.014

IRAS 22449+0757

0.006

0.048
0.013

0.005

0.047

Flux Density (Jy)

Flux Density (Jy)

0.005

0.046

Flux Density (Jy)

0.013 0.013 0.013 0.013 0.012

0.005

0.045

0.004

0.044

0.043

0.004 11000 11200 11400 11600 11800 Heliocentric Velocity (km/s) 12000 12200 12400
5800 6000 6200 6400 6600 Heliocentric Velocity (km/s) 6800 7000 7200
10400 10600 10800 11000 11200 Heliocentric Velocity (km/s) 11400 11600

IRAS 23011+0046
0.028
-0.007

IRAS 23050+0359
0.001

IRAS 23201+0805

0.027

Flux Density (Jy)

0.026

Flux Density (Jy)

Flux Density (Jy)

-0.008

0.000

-0.001

0.025

-0.009

-0.001

0.024
-0.010

0.023 12200 12400 12600 12800 Heliocentric Velocity (km/s) 13000 13200
13500 14000 14500 Heliocentric Velocity (km/s) 15000

-0.002 11000

11200

11400 11600 Heliocentric Velocity (km/s)

11800

12000

IRAS 23204+0601
0.024

IRAS 23327+2913

0.009

Flux Density (Jy)

Flux Density (Jy)
16200 16400 16600 16800 17000 Heliocentric Velocity (km/s) 17200 17400

0.023

0.008

0.023

0.007 0.022

0.006 16000 30500 31000 31500 32000 32500 Heliocentric Velocity (km/s) 33000 33500

FIG. 1: New emission-only HI spectra

20


IRAS 20093+0536
0.060 0.012 0.050

IRAS 20230+1024
0.055

IRAS 20415+1219

0.050

Flux Density (Jy)

Flux Density (Jy)

Flux Density (Jy)
7400 7600 7800 8000 Heliocentric Velocity (km/s) 8200 8400

0.010

0.045

0.040

0.008

0.040

0.030

0.006 0.020 0.004

0.035

0.030 0.025

4500

5000 5500 Heliocentric Velocity (km/s)

6000

7200

4000

4200

4400 4600 4800 Heliocentric Velocity (km/s)

5000

5200

5400

IRAS 20417+1214
0.020 0.018 0.016 0.014 0.012 0.010 0.008
0.002 0.012

IRAS 20480+0937

IRAS 20491+1846

0.010

0.030

Flux Density (Jy)

Flux Density (Jy)

0.008

Flux Density (Jy)
3800 4000 4200 4400 4600 Heliocentric Velocity (km/s) 4800 5000

0.028

0.006

0.026

0.004 0.024

0.006 4000 4500 Heliocentric Velocity (km/s) 5000
8000 8500 9000 Heliocentric Velocity (km/s) 9500

0.050

IRAS 20550+1656

0.026

IRAS 21052+0340
0.028

IRAS 21271+0627

0.048

0.025

Flux Density (Jy)

Flux Density (Jy)

0.044

0.023

Flux Density (Jy)
7500 8000 Heliocentric Velocity (km/s) 8500

0.046

0.024

0.026

0.024

0.042

0.022

0.022
0.040

0.021

0.038 10200

10400

10600 10800 11000 Heliocentric Velocity (km/s)

11200

11400

0.020 7000

0.020 2800

3000

3200

3400 3600 Heliocentric Velocity (km/s)

3800

4000

0.010 0.000

IRAS 21278+2629

0.034

IRAS 21561+1148

0.135 0.130

IRAS 22171+2908

0.032

-0.010

0.125

Flux Density (Jy)

-0.020

Flux Density (Jy)

Flux Density (Jy)

0.030

0.120

0.028

-0.030

0.115

-0.040

0.026
0.110

-0.050 4400 4600 4800 5000 Heliocentric Velocity (km/s) 5200 5400

0.024 8600 8800 9000 9200 9400 9600 Heliocentric Velocity (km/s) 9800 10000

0.105 4000 4500 Heliocentric Velocity (km/s) 5000 5500

0.025

IRAS 22217+3310
0.045

IRAS 22221+1748

0.550

IRAS 22347+3409

0.020

0.040

0.500

Flux Density (Jy)

Flux Density (Jy)

0.015

Flux Density (Jy)
5500 6000 Heliocentric Velocity (km/s) 6500

0.035

0.450

0.030

0.010

0.400

0.025

0.005
0.020

0.350

0.000 6000 6500 Heliocentric Velocity (km/s) 7000

0.300 500 1000 Heliocentric Velocity (km/s) 1500

0.039

IRAS 22387+3154
0.036

IRAS 22395+2000
0.072

IRAS 22402+2914

0.038

0.034 0.032 0.030 0.028 0.026

0.070

Flux Density (Jy)

Flux Density (Jy)

Flux Density (Jy)

0.037

0.068

0.036

0.066

0.035

0.064
0.034 6500 7000 7500 Heliocentric Velocity (km/s) 8000

0.024
0.062

6500

7000 Heliocentric Velocity (km/s)

7500

8000

6500

7000 7500 Heliocentric Velocity (km/s)

8000

IRAS 22472+3439
0.052 0.050 0.048 0.046 0.044 0.042 0.040 0.038 6500 7000 Heliocentric Velocity (km/s) 7500 8000

IRAS 22501+2427
0.014

0.180

IRAS 22575+1542

0.013

0.160

Flux Density (Jy)

Flux Density (Jy)

0.011

Flux Density (Jy)

0.012

0.140

0.120

0.010

0.100
0.009

0.080
0.008 12000 12200 12400 12600 12800 Heliocentric Velocity (km/s) 13000 13200

1600

1800

2000 2200 2400 Heliocentric Velocity (km/s)

2600

2800

21


IRAS 22586+0523
0.018 0.120 0.016 0.100

IRAS 22595+1541
0.028

IRAS 23011+0046

0.027

Flux Density (Jy)

0.014

Flux Density (Jy)

Flux Density (Jy)

0.080

0.026

0.012

0.060

0.025

0.010

0.040

0.024

0.023
2800 3000 3200 3400 3600 Heliocentric Velocity (km/s) 3800 4000 4200 1500 2000 2500 Heliocentric Velocity (km/s) 3000

12200

12400

12600 12800 Heliocentric Velocity (km/s)

13000

13200

IRAS 23024+1203
0.080
0.047

IRAS 23024+1916
0.015

IRAS 23031+1856

0.046

0.015

Flux Density (Jy)

Flux Density (Jy)

Flux Density (Jy)
7000 7500 Heliocentric Velocity (km/s) 8000

0.070

0.045

0.014

0.060

0.014

0.044

0.013
0.050
0.043

0.013
1600 1800 2000 2200 2400 2600 Heliocentric Velocity (km/s) 2800 3000

7000

7500

8000 Heliocentric Velocity (km/s)

8500

0.120

IRAS 23106+0603
0.240

IRAS 23121+0415
0.110

IRAS 23157+0618

0.115 0.220 0.100

0.110

Flux Density (Jy)

Flux Density (Jy)

Flux Density (Jy)
2000 2500 3000 Heliocentric Velocity (km/s) 3500

0.090

0.105

0.200

0.100

0.080

0.180 0.095 0.160 0.090 3000 3200 3400 3600 Heliocentric Velocity (km/s) 3800 4000 0.060 4400 4600 4800 5000 5200 Heliocentric Velocity (km/s) 5400 5600 0.070

0.045

IRAS 23161+2457
0.120

IRAS 23176+2356

0.034 0.032

IRAS 23179+2702

0.040

0.110

0.030

Flux Density (Jy)

Flux Density (Jy)

Flux Density (Jy)

0.028 0.026 0.024

0.035

0.100

0.030

0.090
0.022

7400

7600

7800

8000 8200 8400 Heliocentric Velocity (km/s)

8600

8800

9000

9200

9400 9600 9800 Heliocentric Velocity (km/s)

10000

10200

3600

3800

4000

4200 4400 Heliocentric Velocity (km/s)

4600

4800

IRAS 23179+1657

IRAS 23213+0923

0.100 0.090

IRAS 23252+2318

0.120

0.009

0.008

0.080

Flux Density (Jy)

Flux Density (Jy)

Flux Density (Jy)

0.100

0.007

0.070

0.007

0.060

0.080
0.007

0.050

0.006

0.040
3000 3200 3400 3600 3800 Heliocentric Velocity (km/s) 4000 4200

0.060 1000

1200

1400

1600 1800 Heliocentric Velocity (km/s)

2000

2200

3000

3200 3400 3600 Heliocentric Velocity (km/s)

3800

4000

0.060

IRAS 23256+2315
0.090

IRAS 23259+2208
0.090

IRAS 23262+0314

0.050

0.080

0.085

Flux Density (Jy)

Flux Density (Jy)

0.040

Flux Density (Jy)

0.080

0.070

0.030

0.075

0.060
0.070

0.020
0.050
0.065

0.010 3000 3200 3400 3600 3800 Heliocentric Velocity (km/s) 4000 4200
3000 3500 Heliocentric Velocity (km/s) 4000
4400 4600 4800 5000 5200 5400 Heliocentric Velocity (km/s) 5600 5800

0.050

IRAS 23277+1529

IRAS 23336+0152
0.024

IRAS 23381+2654

0.140
0.045

Flux Density (Jy)

Flux Density (Jy)

0.040

0.120

Flux Density (Jy)

0.022

0.035

0.100

0.020

0.030

0.080
0.018

0.025 3600 3800 4000 4200 4400 Heliocentric Velocity (km/s) 4600 4800

2200

2400

2600 2800 3000 Heliocentric Velocity (km/s)

3200

3400

9600

9800

10000 10200 10400 Heliocentric Velocity (km/s)

10600

10800

22


0.054 0.052

IRAS 23387+2516
0.044

IRAS 23414+0014
0.060 0.042

IRAS 23433+1147

0.050

Flux Density (Jy)

Flux Density (Jy)

0.040

0.048 0.046 0.044 0.042

0.038

Flux Density (Jy)
6000 6500 7000 Heliocentric Velocity (km/s) 7500

0.050

0.040

0.036

0.034 8500 9000 9500 Heliocentric Velocity (km/s) 10000

0.030 3600 3800 4000 4200 4400 Heliocentric Velocity (km/s) 4600 4800 5000

IRAS 23446+1519

0.026

IRAS 23456+2056

IRAS 23471+2939

0.018

0.024

0.020

Flux Density (Jy)

Flux Density (Jy)

0.022

0.016

0.020

Flux Density (Jy)
6000 6500 7000 Heliocentric Velocity (km/s) 7500

0.015

0.014

0.018

0.010
0.012 7400 7600 7800 8000 Heliocentric Velocity (km/s) 8200
0.016

4600

4800

5000 5200 5400 5600 Heliocentric Velocity (km/s)

5800

6000

0.090

IRAS 23485+1952

0.270

IRAS 23488+1949
0.055

IRAS 23488+2018

0.085

0.260

Flux Density (Jy)

Flux Density (Jy)

0.080

0.250

0.075

Flux Density (Jy)

0.050

0.045

0.240
0.070
0.040

0.065 3500 4000 4500 Heliocentric Velocity (km/s) 5000

3500

4000 4500 Heliocentric Velocity (km/s)

5000

5000

5500 Heliocentric Velocity (km/s)

6000

0.031 0.030

IRAS 23532+2513

0.045

IRAS 23560+1026
0.060

IRAS 23564+1833

0.040 0.029

0.055

Flux Density (Jy)
4600 4800 5000 5200 5400 Heliocentric Velocity (km/s) 5600 5800

Flux Density (Jy)

Flux Density (Jy)

0.028 0.027 0.026

0.035

0.050

0.045

0.030

0.040
0.025 0.025

0.035
16500 17000 17500 Heliocentric Velocity (km/s) 18000 18500

4500

5000

5500 Heliocentric Velocity (km/s)

6000

0.100

IRAS 23568+2028
0.024

IRAS 23587+1249

IRAS 23591+2312

0.090
0.022

0.100

Flux Density (Jy)

Flux Density (Jy)

0.020

0.070

0.018

Flux Density (Jy)
4500 5000 5500 Heliocentric Velocity (km/s) 6000

0.080

0.095

0.090

0.060

0.016

0.085

0.014

0.050
0.012

0.080 3500 4000 4500 Heliocentric Velocity (km/s) 5000 5500

2000

2200

2400 Heliocentric Velocity (km/s)

2600

2800

IRAS 23597+1241
-0.024 -0.026

Flux Density (Jy)

-0.028 -0.030 -0.032 -0.034 -0.036 5000 5500 Heliocentric Velocity (km/s) 6000

FIG. 2: Previously detected emission-only spectra

23


IRAS 20210+1121
0.001

IRAS 23410+0228

0.057
0.001

Flux Density (Jy)

Flux Density (Jy)

0.056

0.055

0.000

0.054

-0.001

0.053

-0.001

16000

16500 17000 Heliocentric Velocity (km/s)

17500

27000

27500 Heliocentric Velocity (km/s)

28000

FIG. 3: Non-detections HI spectra

0.028

IRAS 21054+2314
0.016

IRAS 21116+0158

0.066 0.064

IRAS 21582+1018

0.027

Flux Density (Jy)

Flux Density (Jy)

Flux Density (Jy)
3400 3600 3800 4000 Heliocentric Velocity (km/s) 4200 4400

0.026

0.015

0.062

0.025

0.060

0.014

0.058

0.024

0.013 0.023

0.056

0.054 0.022 14000 14200 14400 14600 14800 15000 Heliocentric Velocity (km/s) 15200 15400 0.012 3200 7400 7600 7800 8000 8200 Heliocentric Velocity (km/s) 8400 8600

IRAS 22045+0959
0.072

IRAS 22523+3156
0.164

IRAS 23007+0836

0.028
0.162

Flux Density (Jy)

Flux Density (Jy)

Flux Density (Jy)
6000 6500 Heliocentric Velocity (km/s) 7000

0.071

0.026

0.160

0.158

0.070

0.024

0.156

0.069

0.022

0.154

7000

7500

8000 Heliocentric Velocity (km/s)

8500

0.020 5500

0.152 4000 4500 5000 Heliocentric Velocity (km/s) 5500

IRAS 23254+0830
0.240

0.235

Flux Density (Jy)

0.230

0.225

0.220 8000 8500 9000 Heliocentric Velocity (km/s) 9500

FIG. 4: Spectra with HI emission and absorption components

0.016

IRAS 21442+0007

IRAS 23365+3604
0.068

IRAS 23594+3622

0.016

0.031

0.067

Flux Density (Jy)

Flux Density (Jy)

Flux Density (Jy)

0.015

0.030

0.066

0.015

0.065

0.014

0.029

0.064
0.014
0.028

0.013 21800 22000 22200 22400 Heliocentric Velocity (km/s) 22600 22800
18500 19000 19500 Heliocentric Velocity (km/s) 20000

0.063 9000 9200 9400 9600 9800 Heliocentric Velocity (km/s) 10000 10200

FIG. 5: Spectra HI absorption-only

24


IRAS 23050+0359
0.001

-0.000

Flux Density (Jy)

-0.001

-0.002

-0.003

-0.004 13500 14000 14500 Heliocentric Velocity (km/s) 15000

0.009

IRAS 23327+2913
0.034 0.032

IRAS 23365+3604

0.008
0.030

Flux Density (Jy)

Flux Density (Jy)
31500 32000 32500 Heliocentric Velocity (km/s) 33000

0.008

0.028 0.026 0.024 0.022

0.007

0.007
0.020 18500 19000 19500 Heliocentric Velocity (km/s) 20000

FIG. 6: OH Megamasers

IRAS 21054+2314
0.019

0.028

IRAS 22523+3156

0.026 0.018

Flux Density (Jy)

Flux Density (Jy)

0.024

0.018

0.022 0.017 0.020 5800

14200

14400

14600 14800 15000 Heliocentric Velocity (km/s)

15200

15400

6000

6200

6400 6600 Heliocentric Velocity (km/s)

6800

7000

IRAS 23007+0836
0.131
0.144

IRAS 23121+0415

Flux Density (Jy)

Flux Density (Jy)

0.130

0.142

0.129

0.140

0.138

0.128
0.136

4400

4600

4800 5000 5200 Heliocentric Velocity (km/s)

5400

5600

5800

2200

2400

2600 2800 3000 Heliocentric Velocity (km/s)

3200

3400

FIG. 7: OH Absorbers

25


0.028

IRAS 21054+2314
0.019

IRAS 21054+2314

0.027

Flux Density (Jy)

0.025

Flux Density (Jy)
14200 14400 14600 14800 15000 Heliocentric Velocity (km/s) 15200 15400

0.026

0.018

0.018

0.024

0.023

0.017

0.022 14000

14200

14400

14600 14800 15000 Heliocentric Velocity (km/s)

15200

15400

FIG. 8: HI and OH spectra of IRAS 21054+2314

IRAS 22523+3156
0.028

0.028

IRAS 22523+3156

0.026

Flux Density (Jy)

Flux Density (Jy)

0.026

0.024

0.024

0.022

0.022

0.020 5500

6000 6500 Heliocentric Velocity (km/s)

7000

0.020 5800

6000

6200

6400 6600 Heliocentric Velocity (km/s)

6800

7000

FIG. 9: HI and OH spectra of IRAS 22523+3156

26


FIG. 1e

FIG. 1f

and mapped in the B array, we can infer an upper limit to the size of the IRAS 23327+2913 region to be D1A or D2 kpc in CO-emitting linear scale. To estimate the molecular gas content from the total ÿux 0.009 of CO (J \ 1õ 0) line we adopt the same conversion factor as for the Milky Way galaxy (Bryant & Scoville 1999) M \ 1.20 ] 104F D2(1 ] z)~1 , (1) g CO L where M is the molecular gas mass in M , F is the g _ CO integrated ÿux in Jy km s~1, D is the luminosity distance in 0.007 L Mpc, and z is the redshift. The molecular gas mass derived
0.008 0.006 30500 31000 31500 32000 32500 Heliocentric Velocity (km/s) 33000 33500

for the galaxies in our sample is similar to that found in IRAS 23327+2913 other ultraluminous galaxies (Solomon et al. 1997) and in 0.009 some high-redshift galaxies (Combes et al. 1999) using the same Galactic conversion factor as ours. The 1 p upper limit of the CO ÿux is rms ] *V /(*V /*V )1@2, where 0.008 FWHM FWHM res rms is the noise level in the channel maps, *V is the FWHM line width determined from the Gaussian ïtting to the line 0.008 proïles, and *V is the channel width. The 1 p upper limit res to the molecular gas mass of the companion is then derived following the above equation. For the ULIRGs with 0.007 detected CO emission, the companion may possess a molec0.007 31500 32000 32500 Heliocentric Velocity (km/s) 33000

FIG. 10: IRAS 23327+2913: contour plots, HI 21-cm and OH 18-cm spectra. Contour plots: the left frame is the contour plot of the CO(1-0) emission overlaid on the R-band image, the central frame is the contour plot of the same R-band image at the same scale, and the right frame is the K-band image.

Flux Density (Jy)

27

Flux Density (Jy)


FIG. 11: Radio-FIR Correlation

FIG. 12: HI Mass-FIR Luminosity

28


FIG. 13: HI Mass-Radio Flux

FIG. 14: Dynamic Mass-HI Mass

29


FIG. 15: Dynamic Mass-FIR Luminosity

FIG. 16: Dynamic Mass-Radio Flux

30


TABLE 1: Sample Properties

S IRAS Name (1) (J2000) (2) (J2000) (3) z (4)

60µm

S

1.4GHz

logD25 Morphology (7) S? Sbc HII S? Sy2 Sbc HII/S? Sb/S0-a i (8) 35.63 59.15 46.22 62.80 46.22 39.08 35.63 67.10 72.42 SBb Sb SABa SBb HII/S0-a HII Sy2/E-S0 S? Sa Sy2 S? SBb 35.63 51.93 72.00 66.54 62.80 0.00 37.41 69.22 56.66 33.72 0.00 HII I?/S? Sb Sy1.9 S? Sy2/Sab 43.58 33.72 51.93 44.93 68.71 0.45 0.76 0.9 0.61 1.13 (log 0.1 arcmin) (9) 0.6 0.99 0.74 0.74 0.71 0.96 0.74 1.03 0.91 1.24 0.89 0.97 1.01 0.90 0.84 0.54 1.13 0.94 1.21

(Jy) (5)

(mJy) (6) 5.9 45.8 23.1 15.3 54.6 8.7 19.6 12.2 19.1 38.0 24.3 11.6 24.2 44.0 17.4 12.0 26.8 23.1 29.6 14.3 11.9 30.8 59.0 5.6 14.6

20082 + 0058 20 10 46.29 +01 07 13.6 0.0258 2.69 20093 + 0536 20 11 49.36 +05 45 47.0 0.0175 3.96 20178 - 0052 20 20 28.00 -00 42 36.5 0.0185 3.08 20198 + 0159 20 22 23.07 +02 09 19.1 0.0414 2.40 20210 + 1121 20 23 25.54 +11 31 37.2 0.0564 3.38 20230 + 1024 20 25 30.64 +10 34 21.5 0.0260 2.01 20332 + 0805 20 35 39.16 +08 16 15.8 0.0279 3.11 20369 + 0150 20 39 26.45 +02 01 04.1 0.0132 2.41 20381 + 0325 20 40 39.34 +03 35 47.7 0.0268 2.07 20415 + 1219 20 43 53.46 +12 30 35.4 0.0156 3.18 20417 + 1214 20 44 09.74 +12 25 05.0 0.0147 2.55 20480 + 0937 20 50 29.09 +09 49 05.5 0.0147 2.34 20491 + 1846 20 51 25.90 +18 58 04.8 0.0291 2.79 20550 + 1656 20 57 24.14 +17 07 41.2 0.0365 13.30 21052 + 0340 21 07 45.88 +03 52 40.5 0.0262 2.80 21054 + 2314 21 07 43.36 +23 27 06.4 0.0487 2.23* 21116 + 0158 21 14 12.57 +02 10 41.2 0.0130 4.03 21271 + 0627 21 29 38.93 +06 40 57.3 0.0116 3.11 21278 + 2629 21 30 01.81 +26 43 05.3 0.0161 3.16 21396 + 3623 21 41 41.65 +36 36 47.4 0.1493 2.16* 21442 + 0007 21 46 51.28 +00 21 13.5 0.0741 2.11 21561 + 1148 21 58 36.09 +12 02 19.4 0.0311 2.73* 21582 + 1018 22 00 41.40 +10 33 07.5 0.0271 4.15 22032 + 0512 22 05 47.08 +05 27 16.3 0.0383 2.43 22045 + 0959 22 07 02.05 +10 14 02.7 0.0260 2.88

31


TABLE 1: continued.

S IRAS Name (1) (J2000) (2) (J2000) (3) z (4)

60µm

S

1.4GHz

(Jy) (5)

(mJy) (6) 73.1 11.3 21.4 73.0 33.9 38.9 17.5 13.9 14.5 44.5 7.7 33.6 83.6 14.1 21.0 12.3 81.1 13.9

Morphology (7) SABc SABb S-I/Sc LIN/Sbc SBa;Sy2

i (8) 69.71 75.45 50.88 68.19 37.41

logD25 (9) 1.11 1.17 0.90 1.96 0.96 1.06 0.86 0.75 0.76 0.93 0.81 0.99 1.37 1.21 1.07 0.76 1.14 0.70 1.58 0.90 0.64 0.67 1.09 1.52 1.23

22171 + 2908 22 19 27.94 +29 23 41.6 0.0157 5.86 22217 + 3310 22 24 02.76 +33 26 08.9 0.0220 2.25 22221 + 1748 22 24 33.40 +18 03 56.5 0.0205 2.66 22347 + 3409 22 37 04.67 +34 24 28.0 0.0027 23.10 22387 + 3154 22 41 07.60 +32 10 11.1 0.0242 3.71 22388 + 3359 22 41 12.28 +34 14 57.4 0.0214 8.17 22395 + 2000 22 41 56.03 +20 15 41.6 0.0233 2.56 22402 + 2914 22 42 38.53 +29 30 23.2 0.0242 2.02 22449 + 0757 22 47 28.17 +08 13 37.6 0.0372 2.87 22472 + 3439 22 49 32.17 +34 55 09.2 0.0234 4.98 22501 + 2427 22 52 34.76 +24 43 44.8 0.0421 3.43 22523 + 3156 22 54 45.05 +32 12 47.8 0.0212 2.27 22575 + 1542 23 00 03.60 +15 58 50.8 0.0073 7.23 22586 + 0523 23 01 08.21 +05 39 15.8 0.0115 2.06 22595 + 1541 23 02 00.93 +15 57 51.2 0.0066 4.94 23007 + 2329 23 03 09.28 +23 45 32.3 0.0257 3.64 23007 + 0836 23 03 15.62 +08 52 26.1 0.0162 25.90 23011 + 0046 23 03 41.29 +01 02 38.0 0.0420 2.58

SB0;HII/LIN 58.34 Sy2 HII/S0 S? S? Sbrst LIN 49.79 40.66 40.66 66.54

Sa;Sbrst/Sy2 63.47 Sb/Sbc SAbc Sc SB0;Sy2 S? SABa/Sy1.2 Sm/Sd LIN/SBbc LIN/Sab Sbrst/Sa HII/S? SABa SBbc;HII 64.75 65.36 78.49 51.93 40.66 33.72 43.58 44.93 61.40 56.66 43.58 52.95 71.57

23024 + 1203 23 04 56.63 +12 19 20.6 0.0079 12.80 101.8 23024 + 1916 23 04 56.61 +19 33 08.1 0.0248 7.53 23031 + 1856 23 05 36.16 +19 12 29.6 0.0261 2.09 23050 + 0359 23 07 35.73 +04 15 59.8 0.0474 3.89 23106 + 0603 23 13 12.67 +06 19 23.3 0.0119 4.20 23121 + 0415 23 14 44.00 +04 32 00.8 0.0089 19.30 23157 + 0618 23 18 16.32 +06 35 08.5 0.0165 7.22 44.5 7.4 16.3 11.2 64.3 53.0

SBbc;Sy LIN 64.12

32


TABLE 1: continued.

S IRAS Name (1) (J2000) (2) (J2000) (3) z (4)

60µm

S

1.4GHz

(Jy) (5)

(mJy) (6) 32.5 32.5 25.8 61.4 8.0 20.1 17.5 44.4 21.5 17.4 51.1 56.4 24.2 8.5 67.0 28.8 13.4 37.9 6.5 36.8 31.5 9.8 18.2 19.1 61.2

Morphology (7) SBa Sbrst

i (8) 47.46

logD25 (9) 1.02 0.98 1.09 1.18 0.69 0.61 1.19 1.08 1.04 1.13 1.33 1.10 0.95

23161 + 2457 23 18 38.41 +25 13 58.4 0.0268 4.27 23176 + 2356 23 20 05.65 +24 13 15.9 0.0319 2.41 23179 + 2702 23 20 22.69 +27 18 55.7 0.0145 3.16 23179 + 1657 23 20 30.08 +17 13 32.4 0.0054 9.33 23201 + 0805 23 22 43.92 +08 21 34.7 0.0378 2.33 23204 + 0601 23 23 01.60 +06 18 05.8 0.0560 4.23 23213 + 0923 23 23 53.86 +09 40 02.4 0.0119 4.84 23252 + 2318 23 27 41.28 +23 35 22.5 0.0114 4.91 23254 + 0830 23 27 56.70 +08 46 43.2 0.0289 5.59 23256 + 2315 23 28 06.22 +23 31 52.1 0.0119 3.96 23259 + 2208 23 28 27.31 +22 25 07.3 0.0116 6.59 23262 + 0314 23 28 46.73 +03 30 41.3 0.0171 7.41* 23277 + 1529 23 30 13.57 +15 45 40.6 0.0138 3.11 23327 + 2913 23 35 11.88 +29 30 00.3 0.1067 2.10 23336 + 0152 23 36 14.12 +02 09 18.1 0.0093 10.40 23365 + 3604 23 39 01.24 +36 21 09.0 0.0645 7.09 23381 + 2654 23 40 42.78 +27 10 40.9 0.0340 2.17 23387 + 2516 23 41 16.13 +25 33 03.7 0.0311 3.02 23410 + 0228 23 43 39.65 +02 45 06.1 0.0912 2.28 23414 + 0014 23 44 02.01 +00 3059.5 0.0226 4.47 23433 + 1147 23 45 55.04 +12 03 42.6 0.0142 3.28 23446 + 1519 23 47 09.40 +15 35 49.4 0.0259 4.26 23456 + 2056 23 48 13.77 +21 13 03.5 0.0223 2.29 23471 + 2939 23 49 39.73 +29 55 55.1 0.0176 2.47 23485 + 1952 23 51 04.02 +20 09 00.7 0.0140 4.34

Scd;Sbrst/HII 17.26 SBc;HII/Sbrst 48.65 SAa/ HII Sy 2/S? HII/S? S0 12.25 60.67 33.72 49.79

SAc;HII Sbrst 57.52 SAbc;HII Sy2 33.72 SABbc;Sbrst 53.93

SABc;Sbrst Sy2 43.58 SB0;HII/ Sy1 48.65 SB/Sbab LIN SBb;HII LIN SBa;LIN Sa/S0-a Sb/Sb Sy1/S? SBb Sdm/Scd 48.65 0.00 49.79 37.41 47.46 60.67 35.63 56.66 68.19

1.29 0.60 0.71 0.99 0.39 1.16 1.04 0.87 1.02 1.13 1.24

HII Sy2/SBab 51.93 Sbc S?/Sc 74.39 74.75

SAb;HII LIN 62.80

33


TABLE 1: continued.

S IRAS Name (1) (J2000) (2) (J2000) (3) z (4)

60µm

S

1.4GHz

(Jy) (5)

(mJy) (6) 42.7 71.3 12.5 26.0 18.7 37.7 12.9 33.8 77.6 23.8

Morphology (7)

i (8)

logD25 (9) 1.39 0.94 0.77 1.08 0.82 1.17 0.98 1.16 0.86 1.06

23488 + 1949 23 51 24.90 +20 06 41.3 0.0143 19.00 23488 + 2018 23 51 26.79 +20 35 10.6 0.0178 18.60 23532 + 2513 23 55 49.99 +25 30 21.9 0.0571 2.01 23560 + 1026 23 58 34.09 +10 43 42.2 0.0176 3.26 23564 + 1833 23 59 01.32 +18 50 05.0 0.0179 2.64 23568 + 2028 23 59 25.60 +20 45 00.1 0.0080 4.87 23587 + 1249 00 01 19.87 +13 06 40.5 0.0179 2.02 23591 + 2312 00 01 40.44 +23 29 34.0 0.0145 6.13 23594 + 3622 00 01 58.39 +36 38 56.3 0.0321 4.48 23597 + 1241 00 02 19.08 +12 58 18.0 0.0185 3.39

SBa;HII/Sbrst 60.67 HII Sy2/Sa HII S?/Sbc S?/Sbc SBc/Sbrst S0-a 44.93 62.11 46.22 42.16 29.43 53.93

SBc Sbrst;LIN 71.12 Sy2/S0-a S0 55.78 50.88

34


TABLE 2: HI Emission

Time IRAS Name (1) 20082 + 0058 20093 + 0536 20178 - 0052 20198 + 0159 20210 + 1121 20230 + 1024 20332 + 0805 20369 + 0150 20381 + 0325 20415 + 1219 20417 + 1214 20480 + 0937 20491 + 1846 20550 + 1656 21052 + 0340 21054 + 2314 21116 + 0158 21271 + 0627 21278 + 2629 21561 + 1148 21582 + 1018 22032 + 0512 22045 + 0959 22171 + 2908 22217 + 3310

rms

V

HI -1

V

50 -1

S dv ) (Jy km s (7) 0.6 12.6 5.6 1.1 0.1 1.4 0.4 1.7 2.4 9.9 3.7 1.7 2.3 2.1 1.7 0.5 0.5 1.2 6.8 2.0 1.8 0.5 2.3 8.7 6.3
-1

D

L

log LFIR log LIR log M (L ) (9) 10.68 10.62 10.51 11.11 11.45 10.64 10.82 10.11 10.72 10.44 10.23 10.18 10.92 11.64 10.77 11.26 10.28 10.12 10.47 10.91 10.96 11.00 10.81 10.67 10.55 (L ) (10) 11.02 10.88 10.80 11.38 10.90 10.95 11.07 10.39 10.97 10.71 10.51 10.42 11.18 11.92 11.10 11.58 10.54 10.38 10.74 11.31 11.22 11.28 11.15 10.91 10.81

HI

log M

Dyn

(min) (mJy) SNR (km s (2) 15 15 5 20 10 15 20 10 10 5 10 5 10 10 15 15 20 10 20 15 20 20 15 10 10 (3) 0.30 0.33 0.90 0.37 0.41 0.27 0.26 0.96 0.37 0.49 0.42 0.46 0.31 0.29 (4) 14 149 26 12 36 8 4 19 64 33 22 23 36

) (km s

) (Mpc) (8) 111.9 75.5 78.9 178.8 248.7 112.3 114.6 57.3 115.6 66.2 63.9 62.6 125.6 156.8 112.0 214.5 54.7 49.1 69.0 134.8 114.6 168.9 114.8 65.3 93.5

(M ) (11) 9.27 10.23 9.92 9.93 9.25 9.63 9.05 9.11 9.87 10.01 9.55 9.20 9.92 10.08 9.71 9.76 8.53 8.83 9.88 9.94 9.74 9.53 9.85 9.94 10.11

(M ) (12) 10.99 11.26 11.01 11.25 10.31 11.26 11.33 11.09 11.41 11.71 11.20 10.82 11.74 11.15 10.96 11.34 10.78 11.04 11.22 11.15 11.29 11.76 11.26 11.42

(5) 7784.6 5286.5 5520.0 12301.0 16908.3 7811.3 7967.3 4027.5 8037.5 4640.8 4483.7 4391.2 8715.1 10824.7 7792.3 14667.6 3847.7 3454.2 4837.0 9343.9 7972.3 11638.4 7981.3 4581.8 6528.5

(6) 275.1 323.5 317.6 394.8 100.0 222.1 326.1 430.7 486.7 361.3 364.5 329.2 504.3 282.0 518.2 207.6 519.2 262.3 157.1 240.7 295.4 357.1 563.3 442.8 437.4

0.00027 19 0.28 0.21 0.25 0.63 0.20 0.22 0.31 0.84 0.45 0.35 15 11 28 93 51 51 8 4 66 69

35


TABLE 2: continued.

Time IRAS Name (1) 22221 + 1748 22347 + 3409 22387 + 3154 22388 + 3359 22395 + 2000 22402 + 2914 22449 + 0757 22472 + 3439 22501 + 2427 22523 + 3156 22575 + 1542 22586 + 0523 22595 + 1541 23007 + 2329 23007 + 0836 23011 + 0046 23024 + 1203 23024 + 1916 23031 + 1856 23050 + 0359 23106 + 0603 23121 + 0415 23157 + 0618 23161 + 2457 23176 + 2356

rms

V

HI -1

V

50 -1

S dv ) (Jy km s (7) 7.8 148.1 0.8 1.1 3.3 2.0 0.2 3.7 0.6 4.3 22.8 2.0 24.2 0.6 26.2 0.3 20.5 1.0 0.4 0.5 4.4 30.2 13.5 2.6 7.2
-1

D

L

log LFIR log LIR log M (L ) (9) 10.53 9.85 10.83 11.08 10.61 10.68 11.08 10.97 11.50 10.52 10.14 9.97 9.96 10.87 11.28 11.07 10.40 11.13 10.58 11.42 10.27 10.71 10.80 10.99 10.96 (L ) (10) 10.79 10.06 11.12 11.33 11.01 10.95 11.33 11.21 11.75 10.79 10.39 10.25 10.2 11.12 11.60 11.37 10.74 11.36 10.91 11.67 10.49 10.95 11.05 11.26 11.23

HI

log M

Dyn

(min) (mJy) SNR (km s (2) 10 10 10 20 10 20 25 10 20 25 5 10 5 10 15 15 10 15 15 20 10 5 5 5 5 (3) 0.33 1.08 0.36 0.27 0.39 0.26 0.23 0.36 0.25 0.23 0.58 0.34 0.60 0.29 1.41 0.35 0.37 0.31 0.29 0.28 1.07 0.61 0.66 0.75 0.49 (4) 85 218 13 22 35 36 4 40 22 15 182 25 170 14 7 14 92 13 7 10 27 153 78 21 75

) (km s

) (Mpc) (8) 87.3 11.3 105.2 92.8 102.5 104.2 160.0 102.0 183.9 91.3 31.0 49.2 29.6 111.5 68.6 184.3 33.3 107.0 113.1 208.3 50.2 37.7 70.7 116.7 138.4

(M ) (11) 10.15 9.65 9.34 9.35 9.92 9.71 9.01 9.95 9.67 9.92 9.71 9.06 9.70 9.28 10.46 9.39 9.73 9.43 9.13 9.71 9.42 10.00 10.20 9.91 10.51

(M ) (12) 11.27 11.47 11.50 11.38 11.45 11.66 11.48 11.33 10.84 11.96 10.87 10.88 11.43 10.98 12.07 10.90 11.51 11.25 11.12 11.40 10.06 11.45 11.40 11.31 12.03

(5) 6098.5 800.4 7326.1 6480.6 7144.6 7258.9 11040.4 7107.0 12641.0 6373.9 2190.6 3461.8 2089.6 7758.9 4808.3 12666.5 2352.2 7453.8 7864.1 14258.4 3530.3 2655.6 4952.6 8114.3 9582.6

(6) 358.1 508.1 316.9 345.7 426.0 602.5 348.2 463.5 220.5 724.8 293.3 297.9 692.1 215.2 550.4 160.3 366.3 419.3 425.2 321.3 97.0 455.5 419.2 242.0 257.7

36


TABLE 2: continued.

Time IRAS Name (1) 23179 + 2702 23179 + 1657 23201 + 0805 23204 + 0601 23213 + 0923 23252 + 2318 23254 + 0830 23256 + 2315 23259 + 2208 23262 + 0314 23277 + 1529 23327 + 2913 23336 + 0152 23381 + 2654 23387 + 2516 23410 + 0228 23414 + 0014 23433 + 1147 23446 + 1519 23456 + 2056 23471 + 2939 23485 + 1952 23488 + 1949 23488 + 2018 23532 + 2513

rms

V

HI -1

V

50 -1

S dv ) (Jy km s (7) 3.0 12.0 0.1 0.4 0.4 7.0 2.8 8.0 8.9 5.3 4.8 0.5 13.3 1.3 3.5 0.1 2.4 8.4 0.5 2.3 4.4 5.1 23.7 7.9 3.0
-1

D

L

log LFIR log LIR log M (L ) (9) 10.37 9.94 11.13 11.57 10.32 10.26 11.16 10.21 10.49 10.79 10.27 11.89 10.38 10.91 11.04 11.74 10.86 10.32 10.87 10.71 10.40 10.77 11.13 11.21 11.30 (L ) (10) 10.65 10.22 11.40 11.88 10.57 10.50 11.58 10.52 10.76 11.10 10.55 12.14 10.72 11.23 11.31 10.66 11.12 10.61 11.22 10.95 10.69 10.99 11.36 11.47 11.57

HI

log M

Dyn

(min) (mJy) SNR (km s (2) 10 5 20 20 15 5 5 5 5 5 5 45 5 10 10 20 10 5 10 10 10 5 5 10 30 (3) 0.32 0.45 0.28 0.16 0.28 0.59 0.73 0.58 0.51 0.56 0.41 0.28 0.73 0.35 0.41 0.40 0.42 0.66 0.25 0.35 0.30 0.41 1.37 0.45 0.20 (4) 37 161 5 10 8 105 20 74 76 48 55 10 112 19 30 23 50 29 28 49 50 23 35 28

) (km s

) (Mpc) (8) 60.9 23.0 166.9 245.9 50.9 48.4 127.3 50.5 49.6 73.4 60.1 490.1 39.7 147.2 135.7 412.3 97.0 60.7 113.1 95.6 72.8 60.2 62.2 77.0 256.1

(M ) (11) 9.41 9.18 8.89 9.75 8.34 9.59 10.04 9.68 9.71 9.83 9.61 10.48 9.69 9.83 10.18 9.68 9.72 9.86 9.13 9.69 9.74 9.64 10.34 10.04 10.66

(M ) (12) 11.09 11.72 10.37 11.57 11.16 10.55 11.94 10.88 11.30 11.20 11.04 10.88 11.22 11.57 10.40 11.57 10.89 10.15 11.38 11.22 11.27 12.19 11.22 12.09

(5) 4272.1 1628.5 11502.1 16725.6 3580.7 3404.2 8833.1 3555.3 3488.2 5141.8 4219.5 32145.4 2795.6 10177.0 9403.5 27341.1 6762.8 4262.5 7864.3 6673.1 5268.8 4227.6 4362.5 5392.5 17395.3

(6) 306.1 210.8 122.6 350.9 347.2 181.0 452.1 277.7 306.8 299.1 322.5 488.6 214.6 302.1 465.0 100 436.5 322.2 91.0 457.0 402.1 347.7 815.4 346.8 784.5

37


TABLE 2: continued.

Time IRAS Name (1) 23560 + 1026 23564 + 1833 23568 + 2028 23587 + 1249 23591 + 2312 23597 + 1241

rms

V

HI -1

V

50 -1

S dv ) (Jy km s (7) 4.8 5.2 4.3 3.3 7.3 3.9
-1

D

L

log LFIR log LIR log M (L ) (9) 10.53 10.41 10.01 10.33 10.66 10.57 (L ) (10) 10.80 10.70 10.29 10.6 10.91 10.86

HI

log M

Dyn

(min) (mJy) SNR (km s (2) 5 5 5 5 5 10 (3) 0.25 0.50 0.49 0.38 0.51 0.33 (4) 80 48 106 31 50 39

) (km s

) (Mpc) (8) 74.6 76.8 34.1 75.9 62.2 78.4

(M ) (11) 9.80 9.86 9.07 9.65 9.82 9.76

(M ) (12) 11.20 11.06 10.51 11.37 11.62 11.40

(5) 5227.1 5375.4 2402.4 5317.2 4366.1 5487.7

(6) 302.0 319.6 109.9 357.5 627.5 417.7

38


TABLE 3: HI Absorption Obs. Time IRAS Name (1) 21054 + 2314 21116 + 0158 21442 + 0007 21582 + 1018 22045 + 0959 22523 + 3156 23007 + 0836 23254 + 0830 23365 + 3604 23594 + 3622 (min) (2) 15 20 25 20 10 25 10 5 25 15 rms (mJy) (3) 0.28 0.21 0.31 0.22 0.84 0.23 1.41 0.73 0.30 1.74 SNR (4) 6 8 4 11 1 23 2 8 9 2 V
HI -1

V )

50 -1

)

max

N(HI)/T (cm
-2

s

(km s

(km s

(%) (7) 7.1 12.8 11.0 4.0 3.8 33.0 4.2 2.7 9.2 6.1

K-1 )

(5) 14878.6 4083.6 22255.5 8202.7 7990.6 6260.5 4919.6 8548.0 19318.5 9699.3

(6) 144.4 74.7 98.2 140.9 80.1 197.5 74.0 99.3 276.3 269.7

(8) 1.46E+19 5.04E+18 1.77E+19 4.33E+18 4.47E+18 4.52E+19 4.31E+18 2.82E+18 2.38E+19 1.66E+19

39


TABLE 4: OH Emission F
1665(p eak) 1667(p eak) 1667 -1 1665 -1 1667 -1

Time ( mJy) (5) 2.0 2.0 6.0 19240 368 1.4 32170 4.0 14258 277 325 261 472 (6) (7) (8) (9) ( mJy) (km s ) (km s ) (km s

rms

F

V

V

V

S dv

1665 -1

S dv

1667

log(Lpred ) OH ) (Jy km s (10) 0.2 0.5 (11) 0.5 0.3 1.7
-1

IRAS Name (min) (mJy) SNR (4) 20 8 21

) (Jy km s

)

R

H

(L ) (12) 2.3 3.4 (13) 1.74 2.39 2.45

40

(1)

(2)

(3)

23050+0359

20

0.19

23327+2913

45

0.19

23365+3604

25

0.28


TABLE 5: OH Absorption rms
1667 -1 1665 -1 1667 -1 1665 1667 1665 -1

Obs. Time (mJy) (3) 0.68 0.22 0.85 0.72 5 2623 138 218 6 4870 277 353 1.1 1.0 16 6300 183 210 11.0 10 14750 224 6.4 15.8 1.2 1.6 (4) (5) (6) (7) (8) (9) SNR (km s ) (km s ) (km s ) (%) (%) (Jy km s (10) 8.5 2.2 1.3

V

V

V





dv

dv )

1667

N(OH)/Ts (Jy km s (11) 7.4 11.5 3.4 1.5
-1

IRAS Name

(min)

)

R

H

(cm (12) 1.3 1.5 1.1

-2

K-1 ) (13) 1.74E+15 2.69E+15 8.06E+14 3.50E+14

(1)

(2)

41

21054+2314

40

22523+3156

25

23007+0836

15

23121+0415

5


TABLE 6: OH Nondetections

rms IRAS Name (1) 20082+0058 20093+0536 20178-0052 20198+0159 20210+1121 20230+1024 20332+0805 20369+0150 20381+0325 20415+1219 20417+1214 20480+0937 20491+1846 20550+1656 21052+0340 21054+2314 21116+0158 21271+0627 21278+2629 21442+0007 21561+1148 21582+1018 22032+0512 22045+0959 22171+2908 (Jy) (2) 0.31 0.91 1.00 0.39 0.32 0.44 0.24 0.68 0.28 0.46 0.30 0.40

log(Lpred ) OH (L ) (3) 0.71 0.64 0.48 1.31 1.78 0.66 0.91 -0.07 0.77 0.39 0.09 0.03 1.05 2.04 0.84 1.52 0.17 -0.06 0.43 1.98 1.03 1.10 1.17 0.90 0.71

log(Lmax ) OH (L ) (4) -0.17 0.34 0.10 -0.18 -0.30 -0.17 0.35 1.07 -0.58 -0.07 0.31 -0.18

rms

1612

rms

1720

(Jy) (5) 0.24 0.38 0.80 0.40 0.31 0.45 0.22 0.23 0.23 0.34 0.26 0.41

(Jy) (6) 0.30 0.24 0.42 0.25 0.52 0.46 0.27 0.23 0.23 0.31 0.14 0.49 0.26 0.28 0.23 0.79 -

1 42


TABLE 6: continued.

rms IRAS Name (1) 22217+3310 22221+1748 22347+3409 22387+3154 22388+3359 22395+2000 22402+2914 22449+0757 22472+3439 22501+2427 22523+3156 22575+1542 22586+0523 22595+1541 23007+2329 23007+0836 23011+0046 23024+1203 23024+1916 23031+1856 23050+0359 23106+0603 23121+0415 23157+0618 23161+2457 (Jy) (2) 0.36 0.95 0.35 0.15 0.69 0.27 0.51 0.85 0.36 0.19 0.72 0.42 -

log(Lpred ) OH (L ) (3) 0.53 0.51 -0.42 0.93 1.27 0.62 0.72 1.27 1.12 1.85 0.50 -0.03 -0.27 -0.27 0.97 1.54 1.26 0.33 1.34 0.58 1.74 0.15 0.75 0.88 1.14

log( Lmax ) OH (L ) (4) 0.03 -1.33 0.06 -0.32 -0.59 -0.60 -0.76 0.19 -0.81 0.49 -0.40 -0.09 -

rms

1612

rms

1720

(Jy) (5) 0.39 0.69 0.87

(Jy) (6) 0.33 0.53 0.30 0.24 0.32 0.15 0.16 0.33 0.17 0.18 0.42 0.79 0.29 1.18 0.21 0.29 0.21 0.46 0.59

2 43


TABLE 6: continued.

rms IRAS Name (1) 23176+2356 23179+2702 23179+1657 23201+0805 23204+0601 23213+0923 23252+2318 23254+0830 23256+2315 23259+2208 23262+0314 23277+1529 23327+2913 23336+0152 23365+3604 23381+2654 23387+2516 23410+0228 23414+0014 23433+1147 23446+1519 23456+2056 23471+2939 23485+1952 23488+1949 (Jy) (2) 0.42 0.37 0.34 0.25 0.36 0.44 0.49 0.46 0.19 0.61 0.28 0.45 0.59 -

log(Lpred ) OH (L ) (3) 1.10 0.29 -0.30 1.34 1.94 0.22 0.14 1.38 0.07 0.46 0.87 0.15 2.39 0.30 2.45 1.04 1.22 2.18 0.96 0.22 0.98 0.76 0.33 0.84 1.34

log( Lmax ) OH (L ) (4) 0.48 -0.27 -1.16 -0.60 -0.49 -0.36 -0.33 -0.02 1.22 -0.43 0.92 -0.19 0.08 -

rms

1612

rms

1720

(Jy) (5) 0.51 0.40 0.32 0.64 0.39 0.54 0.41 0.37 0.23 0.67 0.21 0.21 0.24 0.50 0.29 0.38 1.31

(Jy) (6) 0.39 0.44 0.18 0.58 0.53 0.37 0.18 0.28 0.33 0.34 0.26 0.39 -

44 3


TABLE 6: continued.

rms IRAS Name (1) 23488+2018 23532+2513 23560+1026 23564+1833 23568+2028 23587+1249 23591+2312 23594+3622 23597+1241 (Jy) (2) 0.45 0.32

log(Lpred ) OH (L ) (3) 1.45 1.58 0.51 0.35 -0.21 0.23 0.69 1.32 0.57

log( Lmax ) OH (L ) (4) -0.69 -0.12

rms

1612

rms

1720

(Jy) (5) 0.46 0.26 0.44 0.34 0.45 1.35 0.29

(Jy) (6) 0.42 0.44 0.52 0.52 1.33 0.35

45 4


V.

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Acknowledgments I first want to thank my three wonderful advisors at Arecibo, Emmanuel, Tapasi, and Chris, for giving me the opportunity to spend a summer in Puerto Rico, and to work on this pro ject as my senior thesis. I have learned so many things from each of you, and I am really grateful for your help and guidance. Special thanks to the Arecibo Observatory-NAIC for their summer research support and to Sixto Gonzalez. I also want to thank the Department of Physics and Astronomy at Vassar College, in particular Debbie and Fred for being wonderful professors and mentors. Debbie, thanks for teaching me about galaxies, and for being my thesis advisor. Fred, thanks for being a great advisor and international host! I would also like to acknowledge the Office of the President for funding one of my trips to Arecibo. Lastly, I want to thank my family and friends for supporting me throughout my college career. I wouldn't have made it without you.

Familia, los quiero a todos muchisimo... gracias por todo!

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