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Subsections

4 The data

   
4.1 Derived H I parameters

Table 1 presents measured H I parameters for the galaxies detected during our Nançay and Green Bank observations, and the individual spectra are shown in Fig. 2. Criteria for inclusion in Table 1 were partly subjective-i.e., detections with high signal-to-noise and lacking definitive evidence for confusion were always included; however, weaker sources were also included if (1) a positive signal is visible over several consecutive channels and it has a linewidth and line profile shape expected for a real source, or (2) if the detection was corroborated by other workers. Such cases are discussed further in the Notes to Table 1 (Appendix A). Colons (:) following certain entries in Table 1 indicate measurements where the uncertainties may be larger than the formally computed errors.


The columns in Table 1 are defined as follows:


(1) Galaxy name, using the UGC  number from Nilson (1973) or the ESO number from Lauberts & Valentijn (1989) if available, otherwise using the FGC number. The meaning of an asterisk (*), or the letters "a'' and "b'' appended to certain galaxy names are described in Sect. 4.2.

(2) & (3) Right ascension and declination of the optical centers of the targets, in epoch B1950.0, taken from the NED database. These were used as the pointing centers for the H I observations.

(4) Hubble type taken from the FGC when available, otherwise from the NED database.

(5) Galaxy major and minor axis diameters in arcminutes, taken from the NED database.

(6) Spectrum rms, in millijanskys.

(7) Peak flux in the line profile, in millijanskys.

(8) & (9) Raw, measured full width at 20% and 50% of the maximum profile height, respectively, in km s-1. No correction has been applied to the raw linewidths for cosmological stretching, instrumental resolution, or in the case of the Nançay spectra, for the errors arising from describing equal frequency-width channels by a constant velocity width across the entire bandwidth of the spectrum. The latter effect is inherent in the Nançay software, but is negligible compared with our measurement uncertainties.

(10) & (11) W20 and W50 values, corrected for cosmological stretching and spectral resolution, using the relation

\begin{displaymath}W_{w,{\rm cor}}=\left[W_{w,{\rm raw}} + \delta_{\rm c}\right]/(1+z)
\end{displaymath} (1)

(see Haynes & Giovanelli 1994). Here $W_{w,{\rm raw}}$ is the raw observed linewidth at w = 20% or w = 50% peak maximum, $z=V_{\rm h}/c$, and $\delta_{\rm c}$ is given by

\begin{displaymath}\delta_{\rm c}=(0.014\omega - 0.83)\delta_{\rm R}
\end{displaymath} (2)

where $\omega = 20$ and $\omega=50$ for W20 and W50, respectively, and $\delta_{\rm R}$ is the velocity resolution of the measured spectrum (see Bottinelli et al. 1990). No corrections were applied for inclination angle of the source or for turbulent motions.

(12) Heliocentric radial velocity, in km s-1, quoted using the optical convention, $V_{\rm h}=c(\nu_{0}-\nu)/\nu$.

(13) Uncertainty in the heliocentric radial velocity, in km s-1, computed using the prescription of Fouqué et al. (1990):

\begin{displaymath}\sigma(V)=4R^{0.5}P^{0.5}_{W}X^{-1}
\end{displaymath} (3)

where R is the spectral resolution in km s-1, PW=(W20-W50)/2, and X is the signal-to-noise of the spectrum. We define signal-to-noise X as the ratio of the peak flux in the spectrum to the spectrum's rms. According to Fouqué et al., errors in the measured linewidths may be estimated as $\sigma(W_{20})\approx 3\sigma(V)$ and $\sigma(W_{50})\approx 2\sigma(V)$.

(14) Raw, integrated H I flux, in Jy km s-1, after application of an empirically-derived flux calibration scaling factor of 1.26 to the Nançay data (see Matthews et al. 1998a). No corrections have been applied for beam attenuation.

(15) Uncertainty in the integrated line flux, in Jy km s-1, computed using the formula from Fouqué et al. (1990):

\begin{displaymath}\sigma(S)=5R^{0.5}S^{0.5}F^{0.5}_{\rm max}X^{-1}
\end{displaymath} (4)

where $F_{\rm max}$ is the peak flux in the line profile in Jy, S in the raw integrated line flux in Jy km s-1 (taken from Col. 14), and the other parameters are as in Eq. (3).

(16) Corrected integrated line fluxes, in Jy km s-1. For galaxies observed at Nançay, we have computed a correction to our observed fluxes for the finite size of the observing beam using the formula:


\begin{displaymath}S_{\rm c} =
S\left[1+\left(0.75\frac{a_{\rm B}\sin\beta}{\theta_{\rm EW}}\right)^{2}\right]^{\frac{1}{2}}
\end{displaymath} (5)

where S is the raw integrated H I line flux, $a_{\rm B}$ is blue major axis diameter of the galaxy, and $\theta_{\rm EW}$ is the E-W FWHP of the telescope. Because the Nançay beam is elongated, a term is included to account for the position angle of the galaxy, $\beta$ (as measured north to east; see Bottinelli et al. 1990). Our correction assumes a single-peaked Gaussian H I distribution and the empirically-established ratio of H I-to-optical diameter for late-type galaxies established by Fisher & Tully (1975). In addition, since our sample consists entirely of nearly edge-on galaxies, we have assumed that the H I thickness along the minor axis is infinitely thin. A more general form of Eq. (5) applicable to galaxies with arbitrary inclination angles would contain an additional term to correct for the finite extent of the H I layer along the projected minor axis (see e.g, Bottinelli et al. 1990; Matthews et al. 1998a). Position angles used for computing the corrected Nançay fluxes were taken from the FGC, UGC  or ESO catalogues. In cases where there are multiple entries in Table 1 for a single target, no corrected flux is given due to the ambiguity of the angular diameter and position angle corresponding to each of the H I sources. In most instances, the correction derived from Eq. (5) is small ( $\!\!\!~\rlap{$<$ }{\lower 1.0ex\hbox{$\sim$ }}$1%).

For galaxies observed at Green Bank, corrections for beam attenuation were negligible for the present sample. However, for objects observed at elevations $El\le15^{\circ}$, we applied a correction for atmospheric extinction estimated from Fig. 1 of van Zee et al. (1997).

(17) Signal-to-noise ratio of the detected line, defined as the ratio of the peak flux to the spectrum rms.

(18) Notes on individual sources. An asterisk in this column indicates a corresponding note can be found in Appendix A. Other symbols in Col. 18 denote the following:

a: Highly asymmetric profile.
b: Poor baseline.
c: Detected line profile appears to be affected by confusion with a second source.
d: Narrow, dwarf-like line profile.
e: Detection at the edge of the bandpass; measured parameters may be uncertain.
i: Possible interference or contamination from an offband source near the line profile.
n: Noisy line profile.
p: Peculiar line profile.
G: Observations made with the Green Bank 140-ft telescope.

4.2 Investigation of possible source confusions

For each of our detected sources, we queried the NED database over a region surrounding the optical position of the target galaxy in order to identify possible interlopers or confused sources in our H I observations. In events of possible confusion with previously known H I sources, published H I spectra of the possible interloper were compared with our new observations whenever possible. In addition, Digitized Sky Survey (DSS) images of all the regions surrounding detected sources were examined visually for uncatalogued galaxies lying within 1.5$\times$the Nançay or Green Bank FWHP beam dimensions. The results of these searches are described in the Notes to individual objects in Appendix A.

In a few cases we find additional galaxies within our projected beam with angular sizes comparable to or larger than that our target, but without known redshifts. For these galaxies, an asterisk ("*'') is appended to the target name in Table 1 and Fig. 2 to indicate some uncertainty of the identification of our H I detection. The redshifts of these galaxies will require reconfirmation via optical observations.

In situations where we have detected multiple H I sources during observations of a single target and cannot unambiguously resolve which source corresponds to our original target, we list the H I parameters of both detections in Table 1, and designate the two sources with an "a'' and a "b'', respectively, appended to the galaxy's name. Finally, in instances where the systemic velocity of the line profile corresponds closely to that of an interloper with known redshift, the galaxy is declared a questionable detection and is placed in Table 2 (see below), along with an explanatory Note in Appendix B.


Table 3. Undetected sources


Galaxy Name $\alpha$(B1950.0) $\delta$(B1950.0) Type $a\times b$ rms (mJy) Search Range Notes

      (1)

(2) (3) (4) (5) (6) (7) (8)


             

             
FGCE 26 00 10 47.0 -39 00 29 Scd 0.67$\times$0.07 11.3 600-5200 G

FGC 23

00 11 13.0 +43 02 31 Sdm 1.51$\times$0.17 4.54 341-5299,5023-10138  

FGCE 0033

00 14 17.6 -42 35 40 Scd 0.92$\times$0.09 11.4 503-5400 G

FGC 30

00 16 28.2 +26 21 09 Sd 1.01$\times$0.11 3.63,3.81 341-5299,5023-10138  

ESO 294-004

00 18 51.9 -40 44 33 Scd 1.34$\times$0.19 13.0 600-5200 G

FGC 38

00 19 56.2 -10 58 25 Sd 0.76$\times$0.08 2.79 341-5299  

ESO 294-006

00 20 25.4 -42 11 28 Sc 1.12$\times$0.09 12.3 600-5200 G

FGCE 0045

00 21 11.8 -38 56 28 Scd 0.86$\times$0.12 13.3 600-5200 G

ESO 294-011

00 24 59.6 -40 52 54 Scd 1.34$\times$0.19 10.6 1914-6362 G

UGC 263

00 24 34.7 +43 46 39 Sdm 1.48$\times$0.22 3.33,3.67 341-5299,5023-10138  

FGC 63

00 32 55.5 -11 03 17 Sd 0.91$\times$0.10 3.57,3.35 341-5299  

FGCE 82

00 44 35.7 -41 28 47 Sc 1.14$\times$0.09 12.9 600-5200 G

ESO 295-028

00 59 12.1 -40 40 16 Sc 1.05$\times$0.11 16.1 600-5200 G

FGC 132

01 09 47.4 -17 12 49 Sdm 0.81$\times$0.09 4.11,4.16 341-5299,5023-10138  

UGC 786

01 11 46.3 +50 11 05 Sd 1.09$\times$0.15 4.34,4.01 341-5299,5023-10138  

FGCE 157

01 23 28.8 -36 15 27 Sd 1.10$\times$0.09 3.42,5.07 341-5299,5023-10138  

FGC 169

01 25 02.8 -10 39 51 Sd 0.73$\times$0.09 3.11,2.10 341-5299,5023-10138  

ESO 297-013

01 34 25.2 -41 18 18 Sc 1.00$\times$0.13 11.0 600-5200 G

FGC 193

01 45 26.8 +50 38 22 Sdm 0.73$\times$0.10 4.46,4.05 341-5299,5023-10138  

FGC 245

02 04 05.7 +46 01 06 Sd 1.12$\times$0.13 4.23 341-5299  

FGC 269

02 13 12.2 -10 18 50 Sd 1.12$\times$0.12 6.31 341-5299  

FGC 284

02 20 04.6 +17 35 17 Sd 1.01$\times$0.10 7.50 600-5200 G

UGC 1927

02 24 59.3 +43 22 05 Sdm 1.15$\times$0.09 3.98 341-5299  

FGC 298

02 25 42.2 -02 44 21 Sd 1.10$\times$0.09 2.81 341-5299  

UGC 2068

02 32 17.3 +40 40 34 Sdm: 1.09$\times$0.17 3.33 341-5299  

FGC 326

02 36 00.0 +10 33 25 Sd 1.01$\times$0.10 2.94 341-5299  

FGC 333

02 39 19.1 +41 47 11 Sdm 1.04$\times$0.10 3.61 341-5299  

FGCE 260

02 39 39.4 -33 10 02 Sdm 1.01$\times$0.13 13.8 600-5200 G

FGC 362

02 53 11.6 +27 29 40 Sdm 1.10$\times$0.11 3.92,4.57 341-5299,5023-10138 *

FGCE 282

02 57 23.0 -39 47 32 Scd 1.10$\times$0.11 14.2 600-5200 G

UGC 2584

03 09 10.1 +00 51 29 Sd 1.06$\times$0.07 2.25 341-5299  

FGC 418

03 21 16.8 +14 55 32 Sdm 0.90$\times$0.12 3.35 341-5299  

FGC 59A

03 32 10.8 +00 07 47 Sd 1.01$\times$0.17 3.89,3.47 341-5299,5023-10138  

FGC 443

03 38 15.4 +13 24 50 Scd 1.40$\times$0.16 2.82,2.81 341-5299,4559-9658  

FGC 448

03 42 30.8 -04 25 58 Sdm 0.97$\times$0.12 2.96 341-5299  

FGCE 358

03 52 21.7 -41 04 50 Sd 0.58$\times$0.06 14.9 600-5200 G

FGC 67A

04 07 46.4 +00 41 02 Sab 1.01$\times$0.20 3.87,2.80 341-5299,5023-10138  

FGC 472

04 14 35.1 -03 30 28 Sd 0.64$\times$0.07 3.82 341-5299  

FGC 477

04 16 13.4 -15 05 53 Sd 0.65$\times$0.06 2.82,2.99 341-5299,5023-10138 *

FGC 479

04 20 18.3 +30 46 50 Sdm 0.64$\times$0.09 3.11 341-5299  

FGC 480

04 20 19.3 -07 12 22 Sd 0.63$\times$0.09 4.98 341-5299  

FGCE 397

04 22 54.5 -41 44 12 Scd 0.71$\times$0.10 16.5 600-5200 G

FGC 492

04 31 30.1 +01 18 29 Sd 0.92$\times$0.09 4.11 341-5299  

FGC 494

04 32 59.0 -09 02 13 Sd 0.93$\times$0.09 2.83 341-5299  

FGCE 421

04 36 42.0 -22 26 12 Sd 0.59$\times$0.07 3.94 341-5299  

FGC 496

04 39 17.9 +66 57 35 Sdm 0.74$\times$0.09 10.9,3.16 341-5299,5023-10138  

FGC 507

04 47 05.4 +00 23 40 Sd 0.80$\times$0.11 5.21 341-5299  

FGC 522*

05 03 52.5 +85 32 05 Sd 0.99$\times$0.10 ... ... *

FGC 80A

05 05 08.9 -02 02 38 Sm 0.86$\times$0.16 3.31 341-5299  

FGC 532

05 18 23.6 -16 00 59 Sd 0.90$\times$0.11 5.22,6.33 341-5299,5023-10138  

FGC 544

05 46 23.6 -12 31 03 Sd 0.62$\times$0.08 3.80 341-5299  

FGCE 529

05 46 59.4 -17 30 23 Sd 0.87$\times$0.09 3.69 341-5299  

FGCE 535

05 47 48.1 -20 17 51 Sd 0.67$\times$0.09 7.18 341-5299  

FGC 548

05 56 25.7 +60 26 41 Sd 0.74$\times$0.08 5.42 341-5299  

FGCE 552

05 59 34.8 -34 46 56 Sd 0.78$\times$0.07 4.98 341-5299  

FGC 557

06 09 15.8 +53 07 34 Sd 1.19$\times$0.16 4.80,4.07 341-5299,5023-10138  

FGCE 569

06 11 02.0 -34 14 09 Sd 0.90$\times$0.11 3.99,3.67 341-5299,5023-10138  

FGC 559

06 15 22.4 +67 30 41 Sdm 0.86$\times$0.09 6.32,3.53 341-5299,5023-10138  

FGC 564

06 18 41.8 +56 13 52 Scd 1.03$\times$0.10 4.39,3.98 341-5299,5023-10138  

FGC 566

06 22 34.5 +48 43 12 Sd 0.96$\times$0.11 4.18,3.61 341-5299,5023-10138  

FGCE 595

06 23 53.8 -34 23 29 Sd 0.87$\times$0.09 3.39,3.98 341-5299,5023-10138  

ESO 308-012

06 29 30.7 -38 02 03 Sd 0.81$\times$0.11 3.71,5.22 341-5299,5023-10138  

FGCE 602

06 30 03.7 -35 53 08 Sd 0.76$\times$0.09 3.57,4.09 341-5299,5023-10138  

FGC 575

06 30 44.0 +64 43 38 Sd 0.91$\times$0.09 6.71,4.16 341-5299,5023-10138  

ESO 427-007

06 45 41.7 -30 27 44 Sd 1.19$\times$0.17 3.33 341-5299  

FGC 587

06 47 03.9 +45 35 16 Sdm 0.78$\times$0.08 3.79,1.78 341-5299,5023-10138  

FGCE 643

07 10 54.9 -35 23 52 Sd 0.95$\times$0.11 4.52,3.65 341-5299,5023-10138  

UGC 3814

07 18 37.7 +49 22 48 Sm 0.84$\times$0.11 4.42,3.39 341-5299,5023-10138  

FGC 634

07 30 27.8 +20 34 08 Sd 0.64$\times$0.08 4.01 341-5299  

FGC 643

07 33 53.1 +27 06 58 Sm 0.63$\times$0.08 4.67,2.07 341-5299,5023-10138  






 
Table 3: continued
Galaxy Name $\alpha$(B1950.0) $\delta$(B1950.0) Type $a\times b$ rms (mJy) Search Range Notes
      (1) (2) (3) (4) (5) (6) (7) (8)

             

             
FGC 642 07 33 23.2 +59 57 37 Sdm 1.21$\times$0.12 4.54,4.28 341-5299,5023-10138  

FGC 653

07 40 31.8 +60 14 35 Sd 0.81$\times$0.10 5.99,2.88 341-5299,5023-10138  

FGC 673

07 49 43.7 +61 17 08 Sd 1.11$\times$0.09 6.05,5.60,3.18 342-5364,5023-7594,7524-12725  

FGC 676

07 50 52.0 +51 46 14 Scd 1.04$\times$0.10 3.65,3.83,6.52 341-5299,5023-10138  

FGC 705

08 00 48.2 +43 46 41 Sm 0.99$\times$0.10 3.60,1.89 341-5299,5023-10138  

FGCE 687

08 04 26.7 -19 22 24 Sd 0.81$\times$0.09 3.24 341-5299  

FGC 721

08 07 22.7 +49 43 49 Sd 0.86$\times$0.10 4.36 341-5299  

FGC 744

08 18 56.4 +10 29 37 Sd 0.68$\times$0.09 3.18 341-5299  

FGC 758

08 25 04.3 +56 15 31 Sd 0.85$\times$0.09 3.94 341-5299  

FGC 761

08 27 17.3 -19 43 17 Sm 0.78$\times$0.10 4.64 341-5299  

FGC 767

08 29 45.1 +03 40 14 Sdm 0.65$\times$0.09 3.33 341-5299  

FGCE 705

08 31 09.2 -24 28 43 Sd 1.01$\times$0.09 2.57,3.48 341-5299,5023-10138  

FGC 769

08 31 35.9 +59 05 42 Sd 0.76$\times$0.09 4.55 341-5299  

FGC 787

08 40 59.3 -01 38 58 Sd 0.78$\times$0.08 2.97 341-5299  

FGC 788

08 41 18.7 +29 17 09 Sd 0.99$\times$0.09 3.36,2.66 341-5299,5023-10138  

FGC 811

08 51 19.3 +40 12 51 Sd 0.94$\times$0.10 3.52,3.69 341-5299,5023-10138  

FGC 813

08 51 36.3 +52 13 37 Sd 0.85$\times$0.09 4.39 341-5299  

ESO 497-029

09 13 29.7 -23 29 30 Sd 1.66$\times$0.20 4.03,2.64 341-5299,5023-10138  

UGC 4911

09 14 28.3 +54 24 05 Sd 1.12$\times$0.10 5.72 341-5299  

FGC 875

09 17 21.1 +39 26 48 Sd 0.73$\times$0.10 4.63 341-5299  

FGC 912

09 33 00.0 +23 08 49 Sd 0.90$\times$0.09 2.37 341-5299  

FGC 923

09 37 55.8 +31 58 24 Sd 0.96$\times$0.11 3.34 341-2833  

FGC 926

09 38 46.0 +48 19 10 Sd 0.93$\times$0.10 4.31 341-5299  

FGC 959

09 49 36.7 +44 51 37 Sd 1.15$\times$0.08 4.67,3.41 341-5299,5023-10138  

FGC 1049

10 16 05.6 +16 24 04 Sd 0.81$\times$0.10 2.94 341-2833  

FGC 1097

10 30 53.0 +17 59 55 Sd 1.10$\times$0.10 2.02 341-5299  

FGC 1109

10 35 37.9 +70 01 02 Sd 0.67$\times$0.08 5.01 341-5299  

UGC 5815

10 38 29.7 +51 04 25 Sd 1.27$\times$0.10 5.50,5.74 341-5299,5023-10138  

FGC 1124

10 39 36.6 +42 24 41 Sd 0.66$\times$0.09 4.99 341-5299  

FGC 1183

10 59 03.5 +71 16 30 Sd 1.02$\times$0.09 5.99 341-5299  

FGC 1193

11 02 55.0 -09 47 22 Sd 1.01$\times$0.10 4.71 341-5299  

UGC 6226

11 08 36.7 +00 53 57 Sd 1.12$\times$0.10 2.89 341-5299  

FGC 1231

11 17 55.4 +06 31 14 Sdm 1.01$\times$0.11 2.92,5.27 341-5299,5023-10138  

FGC 1263

11 28 24.7 -03 48 20 Sd 0.92$\times$0.10 4.60 341-5299  

FGC 1301

11 42 05.9 +15 02 29 Sd 1.27$\times$0.12 2.54,5.13 341-5299,5023-10138  

FGC 1308

11 45 00.0 +62 17 34 Sdm 0.90$\times$0.10 4.07 341-5299  

FGC 1332

11 53 08.1 +25 11 53 Sdm 0.94$\times$0.10 2.54 341-5299  

FGC 1351

11 59 47.1 +63 23 43 Sd 0.85$\times$0.11 4.66 341-5299  

FGC 1360

12 02 38.9 +40 31 21 Sd 0.88$\times$0.09 3.73 341-5299  

FGC 1370

12 05 07.3 -16 34 12 Sd 0.75$\times$0.10 4.05 341-5299  

FGC 1387

12 11 27.9 +21 55 19 Sd 0.73$\times$0.09 2.70 341-5299  

UGC 7318

12 14 51.3 +49 46 29 Sd 0.94$\times$0.09 4.37,5.96 341-2833,2766-7805  

ESO 574-015

12 34 36.5 -19 14 50 Sd 1.05$\times$0.10 3.65 341-5299  

FGC 1478

12 35 14.9 +74 47 00 Sd 0.93$\times$0.07 6.54 341-5299  

FGC 1483

12 37 11.7 -17 16 04 Sd 0.95$\times$0.09 4.17 341-5299  

FGC 1492

12 40 45.4 +46 07 28 Sd 1.04$\times$0.09 3.26 341-5299  

FGC 1547

13 01 40.0 +54 02 14 Sdm 0.76$\times$0.09 3.24 341-5299  

UGC 8176

13 02 41.0 -00 06 27 Sd 1.09$\times$0.13 3.14,3.40 341-5299,5023-7594  

FGC 1553

13 03 01.7 +25 27 35 Sd 0.93$\times$0.08 3.00 341-5299  

FGC 1559

13 04 07.3 +53 46 56 Sd 0.82$\times$0.10 4.27 341-5299  

FGC 1595

13 17 01.3 +34 44 32 Sdm 1.21$\times$0.17 3.13,2.59 341-5299,5023-10138  

FGCE 1066

13 25 39.3 -19 15 42 Sd 0.90$\times$0.09 3.49 341-5299  

FGC 1635

13 31 23.6 -10 51 03 Sd 0.99$\times$0.07 2.76 341-5299  

FGC 1661

13 41 49.2 +55 12 14 Sd 0.87$\times$0.08 3.71 341-5299  

FGC 1684

13 53 14.4 +79 57 08 Sd 0.68$\times$0.08 8.69 341-5299  

FGC 1686

13 55 02.5 +41 36 32 Sd 0.68$\times$0.09 3.66 341-5299  

FGC 1689

13 55 42.0 +10 30 41 Sd 0.65$\times$0.09 2.78 341-5299  

FGC 1690

13 55 52.4 +29 06 03 Scd 1.46$\times$0.18 3.20,3.27 341-5299,5023-10138  

FGC 1701

13 58 47.8 +43 48 20 Sd 0.80$\times$0.11 3.80 341-5299  

FGC 1708

14 01 51.5 -00 13 01 Sd 0.90$\times$0.10 3.42 341-5299  

FGC 1727

14 10 34.8 -07 12 49 Sm 0.67$\times$0.08 3.34 341-5299  

FGC 1728

14 10 36.0 -06 15 26 Sd 0.62$\times$0.08 2.66 341-5299  

FGC 1739

14 15 16.4 +07 39 17 Sd 0.99$\times$0.09 2.87 341-5299  

FGC 1741

14 15 56.5 -04 55 26 Sd 1.15$\times$0.10 3.01 341-5299  

FGC 1769

14 31 38.9 +09 18 24 Sdm 0.97$\times$0.11 2.76 341-5299  

FGC 1774

14 33 36.1 -02 39 57 Sd 0.86$\times$0.11 3.44 341-5299  

FGC 1783

14 36 05.9 +26 07 19 Sd 0.86$\times$0.09 4.06 341-5299  

FGC 1784

14 36 18.5 +07 50 01 Sdm 0.81$\times$0.10 3.00 341-5299  

FGC 1862

15 09 03.8 +54 38 42 Sd 0.99$\times$0.10 4.75,3.58 341-5299,4559-9658  

FGC 1866

15 12 11.5 +71 26 55 Sdm 0.78$\times$0.10 5.18 341-5299  



 
Table 3: continued
Galaxy Name $\alpha$(B1950.0) $\delta$(B1950.0) Type $a\times b$ rms (mJy) Search Range Notes
      (1) (2) (3) (4) (5) (6) (7) (8)

             

             
FGC 1870 15 12 59.3 -10 16 51 Sd 0.83$\times$0.09 3.01,2.81 341-5299,5023-10138  

FGC 1889

15 19 47.5 +42 04 44 Sd 0.80$\times$0.09 3.49 341-5299  

FGC1904

15 25 58.9 +43 14 20 Sd 0.78$\times$0.10 3.71 341-5299  

FGC 1909

15 28 38.6 +49 11 42 Sd 0.83$\times$0.09 4.08 341-5299  

FGC 1911

15 31 27.5 -09 21 23 Sdm 0.65$\times$0.09 3.39 341-5299  

UGC 9957

15 37 26.3 +40 18 23 Sd 1.12$\times$0.10 3.06,3.04 341-5299,4559-9658  

FGC 1933

15 38 37.9 +06 07 27 Sd 0.88$\times$0.11 3.24 341-5299  

FGC 1936

15 39 33.1 -09 27 32 Sd 0.82$\times$0.09 3.62 341-5299  

FGC 1941

15 40 39.7 +16 56 22 Sd 0.86$\times$0.10 3.29 341-5299  

FGC 1956

15 46 52.9 +71 36 41 Sd 0.72$\times$0.10 4.52 341-5299  

FGC 1966

15 52 07.6 +45 32 51 Sd 1.04$\times$0.09 3.36,3.41 341-5299,5023-10138 *

FGC 1972

15 56 35.2 +41 23 10 Sd 0.91$\times$0.09 5.10 341-5299  

FGC 1990

16 06 15.9 +62 40 11 Sd 0.90$\times$0.09 5.22,6.03 341-5299  

FGC 2006

16 12 41.7 +27 59 08 Sd 0.99$\times$0.12 3.70 341-5299  

FGC 2017

16 16 04.1 +01 16 40 Sd 1.12$\times$0.09 3.04 341-5299  

UGC 10459

16 33 28.6 +41 05 34 Sd 1.67$\times$0.12 3.63,4.18 341-5299,5023-10138  

UGC 10489

16 36 48.7 +62 50 30 Sd 1.57$\times$0.11 6.87,5.73 341-5299,5023-10138  

FGC 2079

16 51 17.8 -04 30 04 Sd 1.23$\times$0.10 4.30,3.36 341-5299,5023-10138  

UGC 10694

17 03 21.7 +43 18 07 Sd 1.15$\times$0.08 6.95 341-5299  

FGCE 1316

18 35 28.5 -42 38 46 Sc 1.10$\times$0.13 11.7 600-5200 G

UGC 11387

18 58 24.0 +42 14 25 Sd 1.12$\times$0.10 6.01 341-5299  

FGCE 1345

19 00 55.6 -38 26 19 Sc 1.43$\times$0.10 12.0 600-5200 G

ESO 337-015

19 11 57.7 -40 55 12 Sc 1.18$\times$0.11 14.2 600-5200 G

ESO 338-001

19 18 33.5 -38 18 04 Scd 1.01$\times$0.10 10.7 600-5200 G

ESO 283-010

19 32 10.3 -44 04 59 Scd 2.06$\times$0.22 16.2 600-5200 G

FGCE 1390

19 37 34.6 -38 29 17 Scd 0.81$\times$0.11 11.9 600-5200 G

ESO 339-005

19 51 37.5 -38 49 47 Sc 1.51$\times$0.20 12.7 600-5200 G

ESO 339-030

19 59 38.4 -41 42 40 Scd 1.18$\times$0.13 14.8 600-5200 G

ESO 340-024

20 20 50.8 -39 12 01 Sbc 0.99$\times$0.11 12.0 600-5200 G

FGC 2270

20 27 32.3 -11 34 43 Scd 1.12$\times$0.10 4.09,3.65 341-5299,5023-10138  

FGC 2272

20 28 59.6 -06 50 34 Sd 0.73$\times$0.08 3.77 341-5299  

FGCE 1504

20 36 44.8 -41 11 28 Scd 0.92$\times$0.12 17.5 600-5200 G

ESO 341-008

20 38 59.3 -42 29 39 Sc 1.15$\times$0.13 11.9 600-5200 G

FGC 2284

20 39 38.9 -04 17 07 Sd 0.68$\times$0.08 4.78 341-5299  

FGC 2285

20 39 48.6 -04 11 23 Sd 0.65$\times$0.08 2.60 341-5299  

FGC 2288

20 45 47.9 -17 25 40 Sd 2.08$\times$0.10 2.67,3.98 341-5299,5023-7594  

ESO 597-039

20 46 44.0 -22 18 17 Sd 1.10$\times$0.11 5.00 341-5299  

FGCE 1543

20 56 30.4 -41 47 13 Sbc 1.66$\times$0.17 14.2 600-5200 G

FGCE 1544

20 57 39.1 -43 00 45 Scd 0.87$\times$0.12 13.2 600-5200 G

FGCE 1552

21 00 41.9 -34 36 13 Sd 0.76$\times$0.09 4.67,3.79 341-5299,5023-7594  

FGC 2312

21 06 27.8 +04 29 06 Sd 0.67$\times$0.06 4.89 341-5299  

FGC 2320

21 19 40.8 -20 25 06 Sd 0.81$\times$0.07 3.05,2.81 341-5299,5023-10138  

FGCE 1631

21 35 26.5 -43 56 06 Scd 0.64$\times$0.09 14.2 600-5200 G

ESO 288-003

21 43 52.9 -42 53 56 Sc 1.21$\times$0.17 12.0 600-5200 G

FGC 2341

21 45 00.7 -12 35 05 Sdm 0.62$\times$0.08 3.78 341-5299  

FGC 2342

21 45 21.2 +25 39 28 Sd 0.67$\times$0.08 3.14 341-5299  

FGC 2344

21 48 40.9 -13 32 19 Sdm 0.81$\times$0.09 3.91,3.43 341-5299,5023-10138  

FGC 2357

21 58 57.6 +03 19 18 Sdm 0.80$\times$0.08 4.03,2.32 341-5299,5023-10138 *

FGC 2369

22 07 21.6 +07 11 01 Sd 0.82$\times$0.10 4.34,3.77 341-5299,5023-10138  

FGCE 1699

22 05 14.9 -38 27 04 Sc 1.08$\times$0.13 18.1 600-5200 G

FGC 2369

22 07 21.6 +07 11 01 Sd 0.82$\times$0.10 4.43,3.77 341-5299,5023-10138  

FGC 2374

22 11 05.9 -14 03 42 Sd 0.73$\times$0.07 5.66,2.39 341-5299,5023-10138  

ESO 345-023

22 30 35.6 -38 02 34 Sd 1.59$\times$0.17 6.08,3.58 341-5299,5023-7594  

ESO 345-037

22 37 30.7 -40 17 30 Scd 1.18$\times$0.15 12.6 600-5200 G

FGCE 1772

22 41 04.7 -38 55 13 Scd 0.78$\times$0.11 10.6 600-5200 G

ESO 291-003

23 08 23.5 -43 07 06 Sdm?sp 2.02$\times$0.20 15.2 600-5200 G

UGC 12536

23 18 31.8 +43 19 35 Sdm 1.19$\times$0.17 3.39,4.64 341-5299,5023-10138  

FGCE 1836

23 33 42.4 -40 21 18 Sd 0.78$\times$0.10 12.0 600-5200 G

FGCE 1868

23 51 57.1 -38 50 33 Sc 1.10$\times$0.11 12.0 600-5200 G


4.3 Marginally-detected, confused, and undetected sources

Table 2 presents the H I parameters derived for marginal or questionable detections. Included in Table 2 are both potential detections of low signal-to-noise, and cases where our detected line profile is deemed likely to result from confusion with a galaxy of previously known redshift. The columns of Table 2 are defined identically to the similarly-headed columns of Table 1. An asterisk in the "Notes'' column indicates an additional note is found in Appendix B.

In Table 3 we list the observed targets for which no clear line signal was detected. The velocity search ranges covered for each target galaxy are listed in Col. 7 of Table 3, along with the rms of the corresponding spectrum in Col. 6. An asterisk in the "Notes'' column indicates an additional note is found in Appendix C, and a "G'' denotes galaxies observed at Green Bank.


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