This manual describes the operation of the Gemini Near-infrared Integral Field Spectrograph (NIFS) from a user’s point of view. It is the primary reference describing the instrument modes, how to prepare for an observing run, how to use the instrument effectively, and how to reduce data generated by the instrument.

2 Applicable Documents

Document ID	Source	Title

3 Introduction

The Gemini Near-infrared Integral Field Spectrograph (NIFS) is the facility near-infrared spectrograph used with the ALTAIR adaptive optics system on Gemini North. NIFS is intended for near-diffraction limited imaging spectroscopy in the 0.94-2.5 mm wavelength range. As such, it is suitable for spectroscopic observations of complex high surface brightness structure, in a spatial or spectral sense, revealed at high spatial resolution by ALTAIR. NIFS records data at a two-pixel spectral resolving power of R ~ 5300. This moderate resolution is sufficient to significantly separate terrestrial OH emission lines. Post-detection OH suppression during data reduction significantly improves sensitivity relative to lower resolution instruments. The moderate spectral resolution is also suitable for dynamical studies of sufficiently high surface brightness astronomical objects.

4 Instrument Overview

This section will provide a general overview of the instrument and its observing modes; AO imaging spectroscopy, AO imaging spectropolarimetry, non-AO imaging spectroscopy, imaging spectroscopy using an occulting disk.

5 Preparing an Observation

5.1 Object Selection

This section will discuss issues that should be considered in selecting suitable objects for observation with NIFS; continuum surface brightness of structure on 0.1² spatial scales, emission-line surface brightness on 0.1² spatial scales, how to access on-line HST images to make these assessments, SNR expectations, saturation limits with and without the ND filter and occulting disks, spatial extent of the source and the need to mosaic, spectral features of interest between OH emission-line, sky subtraction versus dark subtraction strategies, sky determination from the image or via separate sky measurements by nodding the telescope, integration times to reduce the effect of dark current noise, precautions to avoid excessive detector remnance, position angle selection based on rectangular pixel size on the sky, the need to offset from a bright star to acquire very faint objects.

5.2 Guide Star Selection

This section will describe the guide star requirements for ALTAIR, the OIWFS, and the PWFS1 for both the natural guide star and laser guide star modes of ALTAIR. It will describe the operation of gs_search.pl and show how it should be used to identify suitable guide stars and determine their coordinates. It will also discuss likely zero point errors in various coordinate systems and make recommendations about ways of self-consistently defining PWFS1 guide star coordinates and science object coordinates.

5.3 Required Calibrations

5.3.1 AO Imaging Spectroscopy

This section will describe the calibration data that are required to extract scientific results from NIFS AO imaging spectroscopy data; bias frames, dark frames, flat field frames, a spatial calibration frame for correcting image distortion, smooth spectrum star spectra at the same airmass (±5%) for removing atmospheric absorption features, and spectrophotometric flux calibration star spectra. Many science programs will also need to determine the average PSF.

5.3.2 AO Imaging Spectropolarimetry

This section will describe the calibration data that are required to extract scientific results from NIFS AO imaging spectropolarimetry. These will generally be similar to §5.3.1 but will also include calibration of the waveplate polarizing efficiency and orientation (position angle zero point).

6 Operating the Instrument

6.1 Booting the System

This section will describe how to boot the system from a cold start. Visiting observers will not normally have to do this but it will be included for staff astronomers and for completeness.

6.2 Configuring the Science Instrument

This section will describe how to configure the mechanisms of the NIFS IFU spectrograph.

6.2.1 Opening/Closing the Environmental Cover

This section will describe how to operate the environmental cover – mainly as a reminder that this has to be done.

6.2.2 Setting the Focal Plane Mask Wheel

This section will describe how to set the Focal Plane Mask Wheel and will list its contents and the keywords used to identify them.

6.2.3 Setting the Blocking Filter Wheel

This section will describe how to set the Blocking Filter Wheel and will list its contents and the keywords used to identify them.

6.2.4 Setting the Grating Angle

This section will describe how to select the spectrograph grating to be used and how the grating angle can be varied over a small range to optimize the wavelength range recorded.

6.3 Configuring the Science Detector

This section will describe how to configure the NIFS IFU spectrograph detector and the associated Quick Look displays.

6.3.1 Setting the Read Out Method

This section will describe the read out methods of the NIFS science detector and how to select the active read out method. The read out methods offered will be Fowler sampling and linear fitting (integration up the ramp) . It will discuss the pros and cons of resetting the detector at the end of each integration; resetting the array avoids the saturation of bright sky emission lines, but it upsets the stability of the detector and may lead to unacceptably high dark current in subsequent frames.

6.3.2 Setting the Integration Time

This section will describe how to select and set the frame integration time for the NIFS science detector. It will discuss trade-offs between read noise (short integrations), dark current noise (long integrations), and variations in sky emission (on 5 min time scales).

6.3.3 Setting the Number of Fowler Samples

This section will discuss criteria for selecting and the method for setting the optimal number of Fowler samples to obtain at the beginning and end of integrations when using the Fowler sampling read out method. There is a trade-off here between the read noise reduction achieved and the extra dark current noise generated by accessing each pixel multiple times.

6.3.4 Setting the NDR Read Out Period

This section will discuss criteria for selecting and the method for setting the optimal Non-Destructive Read (NDR) period when using the linear fitting read out method. There is a trade-off here between the read noise reduction achieved and the extra dark current noise generated by accessing each pixel multiple times.

6.3.5 Setting the Number of Coadded Frames

This section will describe how to select and set the number of frames that are coadded before data are recorded to disk. Coadding frames is efficient when short integration times are used, but is not likely to be used on typical long integrations on science objects.

6.3.6 Setting the Number of Repeat Sequences

This section will describe how to select and set the number of repeat sequences. A sequence is defined as a basic data set; one set of coadded frames for imaging spectroscopy, but one full set of waveplate positions for imaging spectropolarimetry. Calibration data can usually be obtained more efficiently by recording multiple data sequences. Usually only one data sequence will be recorded on a science object before it is necessary to nod the telescope.

6.3.7 Configuring the Quick Look Display

This section will describe how to configure the science detector Quick Look Display to subtract a sky spectrum, extract and display a 1D spectrum, and display a 2D image over a specified wavelength range.

6.4 Configuring the OIWFS Instrument

This section will describe how to configure the mechanisms of the NIFS OIWFS.

6.4.1 Initializing and Setting the OIWFS X-Y Gimbal Mirror

This section will describe how to initialize the OIWFS X-Y gimbal mirror and how to set its so as to locate an OIWFS guide star.

6.4.2 Setting the OIWFS Filter and Field Stop

This section will describe how to set the OIWFS filter. The OIWFS filter should be set to the same pass band as the NIFS IFU spectrograph in order to minimize differential atmospheric refraction between the OIWFS and science instrument. The OIWFS filter wheel contains sets of identical filters, each with field stops of different diameters. The contents of the wheel will be listed and criteria for selecting the optimal field stop size for a particular application will be described.

6.5 Configuring the OIWFS Detector

This section will describe how to configure the NIFS OIWFS detector.

6.5.1 Setting the Integration Time

This section will describe how to select and set the frame integration time for the NIFS OIWFS detector. The OIWFS should be used for slow flexure compensation when tip-tilt and focus are being sensed by the ALTAIR AOWFS. Relatively long integrations on the OIWFS detector are possible in this mode. However, the OIWFS is used to sense rapid tip-tilt and focus changes when a laser guide star is used with the AOWFS. Integration times in the range 0.01-0.1 s are then required for the OIWFS detector.

6.5.2 Configuring the Quick Look Display

This section will describe how to configure the OIWFS detector Quick Look Display to subtract a sky spectrum and display the resulting image.

6.6 Recording Science Detector Bias Frames

This section will describe how to configure the instrument and record bias frames for the science detector.

6.7 Recording Science Detector Dark Frames

This section will describe how to configure the instrument and record dark frames for the science detector.

6.8 Recording Science Detector Dome Flats

This section will describe how to activate the GCAL flat field lamp, deploy the ISS science fold mirror to point to GCAL, configure the NIFS science instrument, configure the NIFS science detector, and record a sequence of lamp on/off flat field frames.

6.9 Recording an Arc Lamp Frame

This section will describe how to activate the GCAL arc lamp, deploy the ISS science fold mirror to point to GCAL, configure the NIFS science instrument, configure the NIFS science detector, and record a sequence of lamp on/off arc lamp frames for wavelength calibration.

6.10 Recording a Spatial Calibration Frame

This section will describe how to insert the Ronchi grid in the Focal Plane Mask Wheel and record a spatial calibration frame using the GCAL flat field lamp as the light source. This frame is used to determine and correct for image distortion.

6.11 Locating the Occulting Disks

This section will describe how to determine the pixel positions of the occulting disks in the Focal Plane Mask Wheel using the GCAL flat field lamp as the light source.

6.12 Recording OIWFS Detector Bias Frames

This section will describe how to configure the OIWFS and record bias frames for the OIWFS detector.

6.13 Recording OIWFS Detector Dark Frames

This section will describe how to configure the OIWFS and record dark frames for the OIWFS detector.

6.14 Recording OIWFS Detector Dome Flats

This section will describe how to activate the GCAL flat field lamp, deploy the ISS science fold mirror to point to GCAL, configure the NIFS OIWFS, configure the NIFS OIWFS detector, and record a sequence of lamp on/off flat field frames.

6.15 Calibrating the OIWFS X-Y Gimbal Mirror

This section will describe how to initialize the OIWFS X-Y gimbal mirror.

6.16 Recording Science Detector Sky Flats

This section will describe how to configure ALTAIR, deploy the ISS science fold mirror to point to ALTAIR, configure the NIFS science instrument, configure the NIFS science detector, and record a sequence of sky flats.

6.17 Recording OIWFS Detector Sky Flats

This section will describe how to configure ALTAIR, deploy the ISS science fold mirror to point to ALTAIR, configure the NIFS OIWFS, configure the NIFS OIWFS detector, and record a sequence of sky flats.

6.18 Acquiring an Object

This section will describe how to set the ISS rotator angle, acquire a PWFS1 guide star, begin active mirror correction, acquire an OIWFS star, begin tip-tilt and focus correction, view the science field with the telescope acquisition camera, record and display an undispersed object image using the NIFS flip mirror, center the object in the NIFS field using the Quick Look display, acquire the AOWFS star and begin adaptive correction, and spectrally-compress a dispersed NIFS image and display the sky image.

6.19 Focusing the Telescope

This section will describe how to fix the telescope focus that is maintained by the OIWFS.

6.20 Executing a Science Observation

This section will describe how to initiate a science observation and assess the result using the Quick Look Display.

6.21 Recording a PSF Star

This section will discuss considerations in recording a star spectrum with which to determine the PSF.

6.22 Interacting With ALTAIR

This section will describe what is needed to know about interacting with ALTAIR. It will describe how to deploy the ALTAIR feed mirror, set the ISS science fold mirror to point to ALTAIR, locate the AOWFS guide star, how to set the AOWFS integration time and servo-loop parameters, and how to define whether tip-tilt and focus control is derived from the AOWFS or from the OIWFS.

6.23 Interacting With GPOL

This section will describe what is needed to know about interacting with GPOL. It will describe how to insert GPOL into the beam, how to select which waveplate is used, how to select the K band wire grid in NIFS, and how to synchronize data taking with movement of the waveplate.

There are calibration issues here since the GCAL beam will not pass through GPOL or ALTAIR. These will be explained.

6.24 Interacting With GCAL

This section will describe what is needed to know about interacting with GCAL. This may be covered in the sections on recording flat field and wavelength calibration frames. However, there are general issues that need to be described, such as the fact that the GCAL beam does not pass through ALTAIR.

6.25 Checking Science Detector Performance

This section will describe how to record and analyze test data that quantifies the performance of the science detector. Typical ranges of the detector parameters will be listed so that users can determine whether or not the detector performance is optimal. Detector parameters that will be measured are read noise, dark current, remnance, quantum efficiency, and cross-talk. Users who find that the detector is operating outside the acceptable range will be encouraged to contact observatory staff.

6.26 Monitoring Cryostat Temperatures

This section will describe how to monitor the cryostat and detector temperatures and will list typical temperature ranges for these temperatures.

6.27 Initiating the Rapid Warm-Up Sequence

This section will describe how to initiate the rapid warm-up sequence. It will be cautioned that this should only be performed by qualified observatory staff.

6.28 Shutting Down the System

This section will describe how to shut down the system.

6.29 Archiving Your Data

This section will describe how visiting NIFS users can archive their data.

6.30 Summary of Commands

This section will contain a summary list of the commands used to control NIFS that can be used as a quick reference for experienced users.

7 Observing Scenarios

7.1 Jets From Young Stellar Objects

7.2 Massive Black Holes in Nearby Galaxies

7.3 Inner Narrow-Line Regions of Seyfert Galaxies

7.4 Imaging Spectropolarimetry of Cygnus A

8 Data Reduction Procedures

This section will describe the procedures used to reduce NIFS imaging spectroscopy data using IRAF.

8.1 Preparations

8.2 Forming BIAS and DARK Frames

8.2.1 BIAS Frames

8.2.2 DARK Frames

8.3 Linearity Correction

8.4 Defining the Geometrical Calibration

8.5 Combining Object and Sky Images

8.6 Flat Fielding

8.7 Fixing Known Bad Pixels

8.8 Interactively Cleaning Bad Pixels

8.9 Applying the Geometrical Transformation

8.10 Forming Data Cubes

8.11 Extracting 1D Spectra

8.12 Flux Calibration

8.13 Dividing by a Smooth Spectrum Star

8.14 Extracting a 2D Image

8.15 Plotting the Final Spectra

8.16 Deriving Polarization IQU Values

8.17 Plotting Polarization Spectra

8.18 Plotting Polarization Percentage and Position Angle Images

Appendix A: System Performance

This section will summarize NIFS system performance.

Appendix B: Spectrophotometric Standards

Suitable flux calibration stars are listed in Table 1. These stars are drawn from Carter & Meadows (1995, MNRAS, 276, 734), Persson et al. 1998 (AJ, 116, 2475), the UKIRT standards list, and Hunt et al. 1998 (AJ, 115,2594). Only stars brighter than K = 12 mag and bluer than J-K = 0.5 are selected.

Table 1: Spectrophotometric Standard Stars

Star	RA (J2000) Dec		SpT	J	H	K	Ref
HD 590	00 10 16.82	-18 51 45.8	F2V	9.195	8.969	8.947	1
FS 101	00 13 43.58	+30 37 59.9	…	10.553	10.420	10.381	3
HR 9101	00 24 28.44	+07 49 00.2	…	11.622	11.298	11.223	2
FS 2	00 55 09.93	+00 43 13.1	…	10.707	10.509	10.467	3
AS 02-0	00 55 58.60	+39 10 09.0	…	8.775	8.771	8.770	4
HR 9104	01 03 15.94	-04 20 49.1	…	11.045	10.750	10.693	2
FS 104	01 04 59.43	+41 06 30.8	…	10.534	10.437	10.406	3
HD 8864	01 27 29.57	+04 27 43.4	A5	8.631	8.510	8.474	1
FS 107	01 54 10.24	+45 50 37.7	…	10.490	10.286	10.226	3
FS 4	01 54 37.72	+00 43 00.6	…	10.547	10.318	10.279	3
HD 15189	02 26 26.32	-13 52 47.1	G0V	8.460	8.159	8.126	1
HD 15274	02 27 45.52	+08 51 28.6	F5	8.490	8.276	8.250	1
HR 9105	02 33 32.26	+06 25 36.2	…	11.309	10.975	10.897	2
AS 06-0	02 41 03.87	+47 41 22.9	…	8.713	8.694	8.674	4
HD 17040	02 43 40.85	-17 28 53.3	F7V	9.401	9.141	9.107	1
FS 7	02 57 21.17	+00 18 39.4	…	11.102	10.981	10.942	3
FS 108	03 01 09.85	+46 58 47.7	…	10.073	9.795	9.724	3
HD 18847	03 01 24.82	-19 59 13.7	F5V	8.992	8.686	8.653	1
HR 9107	03 32 02.63	+37 20 38.8	…	11.934	11.610	11.492	2
AS 08-0	03 38 08.19	+35 10 53.2	…	8.744	8.723	8.697	4
HR 9108	03 41 02.26	+06 56 15.7	…	11.737	11.431	11.337	2
FS 111	03 41 08.55	+33 09 35.5	…	10.641	10.389	10.282	3
FS 112	03 47 40.70	-15 13 14.4	…	11.203	10.950	10.893	3
AS 09-0	04 11 05.34	+60 10 24.7	…	8.432	8.380	8.340	4
HD 29250	04 35 12.90	-29 38 09.8	A4IV	9.465	9.361	9.354	1
FS 11	04 52 58.84	-00 14 41.5	…	11.341	11.279	11.252	3
FS 119	05 02 57.44	-01 46 42.6	…	9.916	9.873	9.850	3
AS 11-0	05 29 55.50	+39 38 59.0	…	9.151	9.181	9.183	4
HD 37567	05 38 53.86	-12 46 33.3	B8/9V	8.997	8.990	8.993	1
HR 9116	05 42 32.11	+00 09 02.2	…	11.426	11.148	11.077	2
AS 12-1	05 52 21.51	+15 52 41.4	…	11.241	10.931	10.866	4
HD 39944	05 54 43.18	-25 34 39.3	G1V	8.465	8.144	8.104	1
FS 13	05 57 07.55	+00 01 11.1	…	10.491	10.191	10.133	3
HD 40348	05 58 07.11	-02 33 27.9	A0	8.926	8.895	8.892	1
AS 14-0	06 11 24.80	+61 32 12.2	…	8.688	8.623	8.590	4
AS 14-1	06 11 30.03	+61 32 04.7	…	9.871	9.801	9.755	4
HR 9118	06 22 43.86	-00 36 28.9	…	11.723	11.357	11.264	2
AS 15-0	06 40 34.31	+09 19 11.9	…	10.874	10.669	10.628	4
HR 9122	07 00 51.79	+48 29 22.9	…	11.680	11.408	11.356	2
AS 16-2	07 24 15.33	-00 32 47.7	…	11.411	11.428	11.445	4
AS 16-4	07 24 17.56	-00 33 05.8	…	11.402	11.106	11.043	4
HR 9126	07 30 34.49	+29 51 12.1	…	11.876	11.522	11.450:	2
HD 62388	07 43 15.04	-12 24 03.1	A0	8.727	8.691	8.670	1
HD 62998	07 46 07.66	-16 34 37.3	F6V	8.593	8.323	8.294	1
HR 9131	08 25 42.99	+73 01 18.4	…	10.819	10.546	10.499	2
HD 71264	08 26 18.18	-05 51 49.0	A0	8.612	8.565	8.538	1
HR 9134	08 29 25.10	+05 56 08.0	…	11.881	11.624	11.575	2
HR 9135	08 36 12.61	-10 13 36.3	…	12.362	12.098	12.040:	2
AS 18-1	08 51 03.50	+11 45 03.0	…	10.769	10.614	10.575	4
FS 123	08 51 11.78	+11 45 22.8	…	10.173	10.185	10.212	3
AS 19-1	08 51 21.76	+11 52 37.7	…	10.095	9.794	9.746	4
FS 18	08 53 35.42	-00 36 41.3	…	10.812	10.570	10.521	3
FS 125	09 03 20.52	+34 21 02.9	…	10.789	10.428	10.365	3
AS 20-0	09 19 27.66	+43 31 45.7	…	9.551	9.519	9.497	4
HR 9138	09 41 35.91	+00 33 15.4	…	11.354	11.041	10.981	2
HR 9139	09 42 58.33	+59 03 42.7	…	11.683	11.338	11.276	2
HD 84503	09 45 08.58	-26 16 30.5	F2V	8.849	8.638	8.579	1
HR 9141	09 48 56.40	-10 30 32.0	…	11.081	10.775	10.715	2
HR 9142	10 06 28.88	+41 01 24.9	…	11.993	11.729	11.686	2
HD 88449	10 11 40.38	-15 25 25.4	F5V	8.522	8.257	8.223	1
AS 21-0	10 28 42.10	+36 46 18.0	…	9.061	9.043	9.031	4
HR 9143	10 33 51.66	+04 49 04.6	…	12.344	12.121	12.067	2
HD 94949	10 57 49.22	+09 01 07.4	F8	8.267	7.968	7.938	1
HD 100501	11 33 48.19	-29 21 39.3	A9V	9.305	9.119	9.087	1
AS 23-0	12 02 53.41	+04 08 45.9	…	8.889	8.847	8.828	4
HR 9145	12 13 12.00	+64 28 56.0	…	11.958	11.711	11.664	2
HR 9148	12 14 25.40	+35 35 55.0	…	11.642	11.378	11.324	2
HD 106973	12 18 09.33	-01 10 01.6	F8	9.148	8.875	8.836	1
HR 9149	12 21 39.27	-00 07 12.1	…	12.213	11.917	11.861	2
AS 24-0	12 35 15.47	+62 56 56.4	…	9.398	9.345	9.338	4
FS 133	13 15 52.53	+46 06 38.1	…	12.292	11.940	11.868	3
HR 9150	13 17 29.31	-05 32 38.1	…	11.661	11.310	11.250	2
HR 9152	13 58 40.22	+52 06 25.9	…	11.149	10.878	10.831	2
HR 9153	14 07 33.76	+12 23 50.7	…	11.947	11.605	11.560	2
AS 27-0	14 40 06.96	+00 01 45.4	…	10.910	10.781	10.761	4
HR 9155	14 40 57.96	-00 27 45.8	…	12.045	11.701	11.622	2
HD 129540	14 43 13.81	-02 57 31.1	A2V	8.466	8.283	8.247	1
HR 9156	14 51 58.28	+71 43 16.4	…	10.873	10.588	10.523	2
HR 9158	14 58 33.18	+37 08 31.9	…	11.640	11.277	11.210	2
AS 28-0	15 09 20.30	+39 25 49.0	…	8.455	8.378	8.372	4
AS 29-0	15 38 33.41	+00 14 17.9	…	10.234	9.842	9.760	4
HR 9160	15 39 04.17	+00 15 01.9	…	10.914	10.701	10.649	2
HR 9162	15 59 13.65	+47 36 42.5	…	12.258	11.924	11.856	2
HD 147778	16 24 26.00	-17 44 42.0	F0V	8.453	8.151	8.088	1
HR 9164	16 26 42.86	+05 52 23.4	…	12.180	11.895	11.842	2
HD 148332	16 27 23.37	-01 22 27.4	F5	8.480	8.218	8.174	1
FS 138	16 28 06.72	+34 58 48.3	…	10.442	10.413	10.411	3
HR 9166	16 31 33.76	+30 08 46.9	…	11.816	11.479	11.419	2
HD 149226	16 33 28.44	-03 32 04.8	A5	8.006	7.667	7.588	1
HD 154066	17 03 46.49	-12 51 44.9	B8V	7.962	7.845	7.812	1
HR 9169	17 13 44.86	+54 33 18.3	…	11.355	11.118	11.075	2
FS 140	17 13 22.65	-18 53 33.8	…	10.786	10.432	10.360	3
HR 9170	17 27 22.26	-00 19 24.6	…	11.132	10.835	10.739	2
AS 31-0	17 44 06.76	-00 24 57.6	…	10.744	10.644	10.602	4
HD 161961	17 48 36.86	-02 11 46.4	B0.5III	7.369	7.330	7.323	1
FS 141	17 48 59.05	+23 17 43.4	…	11.170	10.879	10.805	3
HD 166733	18 12 08.33	-02 15 29.4	F8	8.495	8.190	8.130	1
FS 35	18 27 13.48	+04 03 09.8	…	12.194	11.840	11.739	3
AS 32-0	18 36 10.5	+65 04 30.0	…	8.017	7.917	7.925	4
HR 9177	18 39 33.87	+49 05 37.6	…	12.104	11.764	11.688	2
FS 147	19 01 55.27	+42 29 19.6	…	9.910	9.883	9.865	3
HR 9178	19 01 55.40	-04 29 12.0	…	10.966	10.658	10.566	2
AS 34-0	19 17 34.59	+48 06 03.2	…	8.443	8.434	8.436	4
FS 148	19 41 23.43	-03 50 57.2	…	9.509	9.490	9.477	3
FS 149	20 00 39.15	+29 58 37.4	…	10.104	10.082	10.086	3
HD 193727	20 22 15.40	-16 06 49.0	F0V	8.977	8.826	8.783	1
AS 35-0	20 35 11.20	+36 08 49.0	…	8.625	8.544	8.524	4
FS 150	20 36 08.40	+49 38 24.4	…	10.157	10.009	9.956	3
HR 9182	20 41 05.42	-05 03 42.6	…	11.479	11.142	11.082	2
HR 9183	20 52 47.41	+06 40 03.9	…	12.247	11.940	11.873	2
HD 201916	21 12 35.11	+00 53 36.2	F0	7.999	7.819	7.786	1
FS 151	21 04 14.82	+30 30 21.6	…	12.206	11.943	11.869	3
HR 9185	22 02 05.66	-01 06 01.6	…	12.0