The ALMA Site

The meteorological conditions on Chajnantor have been monitoried since April 1995. In the period 1995-2004, the data was collected using the NRAO and ESO weather stations and since 2004 similar data has been collected at the weather station at the Atacama Pathfinder EXperiment  (APEX).  The former data can be downloaded from the page https://science.nrao.edu/facilities/alma/site, which also contains a very detailed description of the site characteristics and links to publications in the ALMA memo letter series, and the latter data can be downloaded from http://archive.eso.org/wdb/wdb/eso/meteo_apex/form

Figure 3 shows the temperature, humidity, wind speed, and barometric pressure on Chajnantor as function of time of the year. The southern hemisphere winter (June-August) is characterized by lower temperatures, lower humidity, higher wind speeds, and slightly lower pressure compared to the southern hemisphere summer (December-February) conditions.

The quartile data in the figures are based on median values per each hour. The median filter tends to smooth the appearance. The smoothing of the data affects in particular the plot of the wind; in the raw database measurements there are wind gusts of up to 46 m/s, and sustained wind for more than one hour of up to 32 m/s.

Figure 3: Weather statistics (temperature, humidity, wind speed, and pressure) measured at the APEX weather station. Data have been collected over the years 2006-2010. The blue, green, and red bars show the 1st, 2nd, and 3rd quartile of the data. The raw data have a dump rate of 1 minute. From the raw data, the median value per hour was calculated and these median values were sorted per weeks. The thin cyan line shows the tenth largest value in the database, and the thin purple line shows the tenth lowest value among the median values, per week, respectively.

Figure 4: Diurnal variation of temperature (upper row) and wind speed (lower row) in June (left column) and December (right column) as function of Chilean local time (CLT). Data have been collected over the years 2006-2010. The blue, green, and red bars show the 1st, 2nd, and 3rd quartile of the data. The raw data have a dump rate of 1 minute. From the raw data, the median value per hour was calculated and these median values were sorted per time intervals. The thin cyan line shows the tenth largest value in the database, and the thin purple line shows the tenth lowest value among the median values, per time interval.

The diurnal variation of temperature and wind in a representative winter month (June) and in a representative summer month (December) is shown in Figure 4. Typical night-time temperatures range from  -10 to -6 degrees C during winter and -4 to 0 °C during summer. Temperature rises slowly after sunrise, reaching normally around -4 °C during winter time and +4 °C summer time.  Extreme night and day temperatures range from a minimum of -20 °C to a maximum of 12 °C, respectively.

During winter, the wind speed at night time is characterized by steady wind 5-7 m/, increasing after sunrise, reaching 6-11 m/s at 12-14 (CLT), after which the wind speed begins to drop slowly. The wind speed during summer looks slightly different, with a minimum of 2-4 m/s at 22-02 (CLT), gradually increasing up to 19 (CLT), when it reaches 8-10 m/s, after which the wind speed drops relatively abruptly. The latter winter speed pattern normally starts in October and continues until March.

PWV and Atmospheric Transmission

At millimeter and submillimeter wavelengths, pressure broadened molecular spectral lines make the atmosphere a natural limitation to the sensitivity and resolution of astronomical observations. Tropospheric water vapor is the principal culprit. The translucent atmosphere both decreases the signal, by attenuating incoming radiation, and increases the noise, by radiating thermally. Furthermore, inhomogeneities in the water vapor distribution cause variations in the electrical path length through the atmosphere. These variations result in phase errors that degrade the sensitivity and resolution of images made with both interferometers and filled aperture telescopes.

Figure 5 shows the precipitable water vapor (PWV) measured by the APEX radiometer as function of the time of the year. This image shows that during more that 50 % of the time between April and December, the PWV is below 1 mm (green quartile), and during the 5 best months (May-September), the PWV is below 0.5 mm for more than 25% of the time (blue quartile). The instrument uptime was in this period 80%. Lack of data indicate that the shutter was closed due to high humidity, and during these periods the pwv is assumed to be 10mm.

Figure 5: The precipitable water vapor, measured by the radiometer at APEX, as a function of the time of the year. Data presented here have been collected over the years 2007-2010. The blue, green, and red bars show the 1st, 2nd, and 3rd quartile of the data.

Figure 5 shows that the 1^st, 2^nd, and 3^rd quartile of the PWV in March is 1.6, 3.3, and 5.2 mm, respectively, and the corresponding quartiles for August is 0.4, 0.65, and 1.05 mm.  The transmission plots at these PWVs is shown in Figure 6. This image shows that in March, it is fully possible (from a transparency point of view) to operate in most frequency ranges in the lower frequency ALMA bands, and in August, the upper frequency ALMA bands open up as well.

Figure 6: The zenith atmospheric transmission in March (upper panel) and September (lower panel) represented by the 1^st, 2^nd, and 3^rd quartile of the PWVs in the two months, respectively. The different colored boxes are the ALMA bands 3-10.

Figure 7: The diurnal variation of the PWV in March (upper panel) and August (lower panel).

The PWV also has a diurnal pattern. Taking March and August 2010 as two examples of an (late) Altiplanic month and Southern winter month, respectively, it can be shown (see Figure 7) that the PWV peaks at 19 (CLT) in both winter and summer, but the absolute scale differs; During 50% of the time in March 2010 the PWV was below 1.8 mm, and during August 2010, the PWV was below 0.7 mm 50% of the time. It should however be noted that these numbers vary greatly from year to year.

Phase Fluctuations/Stability at Chajnantor

Tropospheric phase stability was measured directly using two phase monitors (site test interferometers, STI), one built by NRAO and one by ESO, and located in Chajnantor. These observed unmodulated beacons broadcast from geostationary satellites and measure the phase difference between the signals received by two 1.8 m diameter antennas 300 m apart. Because the atmosphere is non-dispersive away from line centers, the results can be scaled to millimeter and submillimeter wavelengths. From the phase time series, the RMS path fluctuations on a 300 m baseline, the power law exponent of the phase structure function, and the velocity at which the turbulent water vapor moves over the array were obtained. The NRAO STI operated almost continuously since May 1995 until August 2005, and the ESO STI from June 1998 until July 2005. The data is analyzed to derive the path fluctuations AT THE ZENITH for a 300m baseline using 10 minutes time bins, to guarantee that the phase screens have had enough time to cross over the STI baseline completely.

The results of both STIs are as follows (fluctuations at zenith for 10 minute bins):

A merged statistical plot of the information obtained with the NRAO STI is as follows:

The plots in the upper row (from left to right) show the monthly median, the comparison of the monthly median as a function of year and the median diurnal variation of the path fluctuation RMS, respectively. There is a clear correlation of increased phase fluctuations with Altiplanic winter and with time of day (larger fluctuations during day time, peaking near local noon).

The plots in the lower row (from left to right) show the cumulative distributions of the fluctuations, the slope of the dependency of the fluctuations with baseline lenght and the crossing time of the STI baseline, respectively. The plots suggest that the fluctuations are never pure Kolmogorov, and that a possible mixture of layers, different layer velocities, etc may be occurring at the AOS.

References:

Otarola A., Holdaway M., Nyman L-E., Radford S.J.E., Butler B. J (2005-02-01), ATMOSPHERIC TRANSPARENCY AT CHAJNANTOR: 1973-2003, ALMA Memo # 512

Neal Evans, John Richer, Seiichi Sakamoto, Christine Wilson, Diego Mardones, Simon Radford, Selby Cull, Robert Lucas (2005-07-03), Site Properties and Stringency, ALMA Memo # 471

Alison Stirling, John Richer, Richard Hills, Adrian Lock (2005-04-05), Turbulence Simulations of Dry and Wet Phase Fluctuations at Chajnantor. Part I: The Daytime Convective Boundary Layer, ALMA Memo # 517