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Produced by the NASA Center for Aerospace Information (CASI)
CRW, fix. --4, F

ry

t : -CR-175103) OPTICAL THICKNESS AS N84 -1CO28

RB,- ED TO POLLUTANT EPISODES AND THE

C:UNC:ENTRATION OF VISIBILITY DEGRADING

EULLUiANTS Final heport, Nov. 1981 - Nov. Unclas

1982 (Miami Univ.) 50 p HC. A03/MF A31 G3,145 12507

OPTICAL THICKNESS AS RELATED TO POLLUTANT EPISODES

AND THE CONCENTRATION OF VISIBILITY DEGRADING POLLUTANTS

Joseph M. Prospero, Dennis Savoie,

Thomas Snowdon, Paul Ewbank

Rosenstiel School of Marine and Atmospheric Science

University of Miami

4600 Rickenbacker Causeway AQ^^ ^^ '^^'?Q

Miami, FL 33149-1098

a^ 

MAC ^aaA

EO

r ^^CS ^ FpG\^'r

r^ t^'^^gg D^^

June 1983

Final Report for Period November 1981-November 1982

`a

Prepared for

GODDARD SPACE FLIGHT CENTER

Greenbelt, Maryland 20771
. Report No. ^2. GovernmeAt Accession No. 3. Recipient's Catalog No.

4. Title and Subtitle 51 Repovi Date

Optical Thickness as Related to Pollutant April 1983

Episodes and the Concentration of Visibility 6. Performing Orgonkation Code

ygradi ng Pollutants--

7. Auther(s) Joseph M. Prospero, Dennis Savoie, 8. Performing Organization Report No.

Thomas Snowdon, Paul Ewbank

'9. Performing Organization Name and Address 10. Work Unit No.

Rosenstiel School of Marine & Atmospheric

Science, University of Miami tt. Cantraetarcran ► Na.

4600 Rickenbacker Cswy, Miami, FL 33,149 NAS5-26768

13. Type of Report and Period Covered

12. Sponsoring Agency Name and Address Final Report

Goddard Space Flight Center November 1981 -

Greenbelt, Maryland 20771 November 1982

4. Sponsoring Agency Code

Dr. Robert S. Fraser, Code 915

15;T4upPU entory Notes

16. Abstract

A network of six sun photometers was placed in the central and

northeast United States during the months of July through October,

1931. The objective of the program was to obtain measurements of

atmospheric turbidity which can be related to the concentration of

visibility-degrading pollutants in the atmosphere. These measurements

will serve as ground truth for a program (R. Fraser, NASA/Goddard) to

develop remote sensing techniques for measuring the vertically integrated aerosol concentrations in pollution episodes.

The sun photometers measure the direct solar radiation in four

passbands: 380 nm, 500 nm, 875 nm and 940 nm. The first three

passbands will be used for measuring -the aerosol optical depth and the

last for measuring precipitable water.

Stations were established in: St. Louis, Missouri; Columbus, Ohio

State College, Pennsylvania; Philadelphia, Pennsylvania; Narragansett,

Rhode Island; Greenbelt, Maryland.

17. Key Words (S. t ected by Author(s)) 18. Distribution Statement

Aerosols, aerosol optical depth,

pollution episodes, atmospheric .

turbidity, remote sensing.

19. Security Clossif. (of this report) 20. Security Clossif. (of this page) 21. No. of Pages 22. Price'

y
i

4

TABLE OF CONTENTS

Introduction ... ..............................p 1

Sun Photometer Calibrations :, .................. 2

Data Processing .^ .............................

Discussion ...... 8

Goddard . ............ ...................i. 10

Phil adelphia ............................. 11

Rhode Island ............................. 13

Penn State ............................... 15

St. Louis ................................ 16

Columbus, Ohio ........................... 17

/y Con c 1 u s i o n . . . . . . . . . . . . . . . . . . . . . . . . . • . . . . . . . . . . 1 z,

Tables 1 - 4 .................................. 20 - 26

Appendixes I - V

Report. of Inventions and Subcontracts
LIST OF TABLES

Table 1 Sun Photometer Calibration

Constants for Three

Calibration Periods 20

Table 2 Recommended Sun Photometer

Calibration Constants 21

Table 3 Error Sensitivity in Alpha:

Effect on Alpha of an Error

of 0.01 in T with rG

Constant R 22

Table 4 Number of Observations Per 

Day at Each Station 23 26

r

61

M

g 

,, . .._ -,r-.-`:. -i.^ ^-^. ^- ►tea
t 

W . .

Introduction

A sun photometer network was established in the northeast

United States during the late summer and early fall of 1981.

The photometers were used to make measurements of aerosol

optical depth at selected time intervals. These measurements

serve as a data base for the development of an algorithm for

the measurement of aerosol optical depth from satellite

systems.

The sun photometer instrument used is a four-channel

device which incorporates interference filters centered at

380 nm, 500 nm, 875 nm and 940 nm. The 940 nm passband is

used for estimating precipitable water. The other three are

selected for aerosol measurements. The instrument is a

hand-held device with a digital readout display and a

peak-hold circuit to facilitate measurements. A detailed

description of the instrument and the observing techniques

employed is found in Appendix I (Sun Photometer Measurements

- Instructions to Observers).

The photometers were distributed so as to obtain good

coverage in the northeast portion of the United States, an

area which is often affected by dense pollutant hazes. The

selected sites are: St. Louis,. Missouri; Columbus, Ohio;

State College, Pennsylvania; Philadelphia, Pennsylvania;

Narragansett, Rhode Island; Greenbelt, Maryland. A list of

station locations and observers is found in Appendix II.

-1- 
t

The data gathering protocol calls for a sequence of a

minimum of four, to a maximum of seven readings; these were to

be made in the m+;rning at specified time intervals. The time

intervals were be selected so as to provide a good range of

sun angles during the mornin g, from about 0700 AM LST until

about 1200 LST (see Appendix I).

Observers were paid for the observations that they made

according to a fixed schedule (see Appendix III, Cover Letter

to Observers). As an inducement to the observers, prizes

were offered to the persons who recorded the greatest amount

of data.

All instruments were thoroughly inspected and intercompared prior to going into the field. At the completion of

the experiment, the instruments were recalibrated in Miami.

Data was recorded on a standard form (see Appedix IV).

Data was returned to Miami at the end of each week by means

of pre-addressed, post-paid envelopes.

Sun Photometer Calibrations

The instruments were calibrated on three occasions:

J) November and December, 1980; 2) June and July, 1981, and

3 ) April, 1982.

1. The calibrations in November and December, 1980,

were carried out at the completion of a previous

major field program. For this purpose a Langley
calibration was carried out in Miami on instrument

UM 322 which wac then used as the reference

standard. All other instruments were calibrated

against UM 322 using neutral density filters.

2. The calibrations of June and July, 1981, were merely

a recheck against UM 322 to verify performance prior

to sending the instruments out into the field for

the contract experiment.

3. The calibrations of April, 1982, were an intensive

cross check between UM 322 and UM 323 against all

other photometers

The University of Miami sunphotometer UM 323 had been

sent to NOAA/GMCC, Boulder, Colorado to be used in an

extensive intercomparison study of sunphotometers from a wide

range of sourcej and institutions. The intercomparisons were

carried out under the supervision of E. Dutton and J.J. de

Luisi from 19 October through 4 November 1981. During that

period, extensive data were obtained at frequent time

intervals at relative air masses (M) ranging up to 20 on six

days. On half of those days, however, readings were possible

only during the morning or the afternoon as a consequence of

the presence of clouds during the balance of the day.

For each of the half-days, the raw data for the blue,

green, and red channels were plotted as a Langley plot (i.e.,

t
S

-4-

the natural log of the instrument response versus the 

relative air mass, (MD. For the water channel, lnQ (where Q

is the response in the water channel divided by that of the

4 red channel) was plotted versus the square root of M. Each

of the plots was visually examined for obvious outliers

and/or nonlinearity; the outliers and the data obtained

during periods of obviously changing turbidity were deleted

from the final data sets. Regression analyses were performed

on each of the final data sets to determine the apparent lo's

and Q for the .instrument.

For each day of the three days in which both morning and

afternoon data were obtained, it was apparent that the

turbidity was either increasing or decreasing slightly

throughout the day. With a constantly increasing turbidity,

the apparent I o 's from the morning data will underestimate

the true Io while those from the afternoon data will

overestimate it; the opposite is true in the case of

decreasing turbidity. The best estimate of the true 1 is

obtained from the mean of the highest underestimate and the

lowest overestimate, which are generally within a percent or

two of one another.

The best estimate of the I o 's and Q o for photometer

UM323 from the Boulder data (1981) are given below along with

the estimates obtained from the calibration against UM 322 in

1980.
Channel 1981 1980

Blue 1 (380) 39.1 (*2%) 39.2

Green I0(500) 184.3 (*.5%) 182.5

Red I0(875) 125.8 (+.4%) 125.7

Water 4o(945) 2.03(+ 3%) 2.06

The 1981 results are in excellent agreement with those of

1980, indicating that no significant alteration in instrument

response had occurred during the one year period.

In Table 1 we summarize the calibration constants for

all instruments as determined in each of the three

calibration runs. For the most part, the instruments

performed reasonably well. The maximum range of values for

the three calibrations for any one instrument was generally

less than 2 06 for the red and green channels. The blue

channel was considerably worse with an average change of 6%.

The apparent change in calibration constants is

attributable to a number ^,f factors. First of all, we are

comparing, in effect, calibrations derived from two

independent "prime" calibrations, that of UM 322 in Miami in

Period 1 and that of UM 323 at Boulder. Shaw, in his article

on sun photometril, (Bull. Amer. Meteorol. Soc. 64, 4-10,

1983), points out the severe problems of doing Langley plots

in continental environments. He states that one can easily

get "excellent" Langley plots that are in reality not

excellent. That is, the aerosol content builds up or falls

off in a systematic manner so that one gets a deceptively

"good" straight line in the Langley plot. For example, Shaw

-5-
finds that Langley calibrations performed by him at Tucson

show consistently lower to values by 1 to 3% than

calibrations perfo l ;med at Mauna Lo y . Consequently, he

recommends that tho only good way to do calibrations is at a

site such as Mauna Loa; these measurements should be made

concurrently with aerosol measurements to ensure that the

aerosol concentration does not change. Unfortunately, we

could not do our calibration at Mauna Loa.

Another problem has to do with the fact that we had to

send instrument UM 323 to Boulder for the intercomparison;

we could not part with our "prime" reference, UM 322, for an

extended time. Thus; we had to transfer the UM 323

calibration through UM 322 to the other instruments. This

problem was exacerbated by the fact that the Boulder

intercomparison lasted much longer than anticipated. Thus we

could not carry out our final calibration transfer until some

six months after the field experiment had been completed.

The relatively poor response of the blue channel is 

disturbing but not completely unexpected. The transmssion

through the filter is so low that we must use the maximum

gain of the integrated photo-detector/amplifier. Also, as

Shaw also notes, the photometers are subject to much greater

drifts, about 1% per year, in the blue wavelengths than in

the longer wavelengths. Also, we have experienced problems

with deterioration of the blue filters.

-6-
Despite the fact that the blue channel performance is

being pushed to the limit, a perusal of the data indicates

that it did perform satisfactorily. For example, on a number

of days data was obtained at Goddard Snace Flight Center

using sun photometer No. 320 at frequent intervals beginning

very early in the morning. On many of these days, the blue

a

channel was yielding initial readings of 0.0 and .1 (i.e.,

the minimum resolvable reading); over the following hour or

two these readings would increase dramatically as the solar

elevation increased. Despite the extremely low initial

readings the computed turbidities in the blue channel and the

resulting alpha values were often remarkabl y constant: over

that time interval. An example is August 5 when readings

began at 7:12 AM. The initial readings in the blue charnel

were 0.1 and 0.0. Readings were subsequently taken every few

minutes and the readings in the blue channel increased to

values of about 5. Over the course of the approximately 4

hour set of readings, the computed turbidities in the blue

channel were remarkably consistent as were those in the green

and red channels. This set of readings attest to the

stability and linearity• of the blue channel even in the

extreme low end of its range. Another data set from Goddard

on August 28 yields a similar validation of performance in

the blue channel.

4

-7-
The final selection of calibration constants are

presented in Table 2. These values are the means of fthe

calibration constants obtained in calibration periods 2 and

3; that is, the ones before and after the field program.

Data Processing

The data received from the field stations was

transferrer) to punched cards. These values were converted to

aerosol optical de p th. The computation incorporates a

correction for the temperature coefficient of the sun

photometer detector. All data print outs have been checked

for obvious errors and the y have been corrected accordingly.

Copies of all data have been delivered to Dr. Bob Fraser in

both punched card form and as computer print-out that

presents all input data as well as the computed values of

aerosol optical depth and alpha (the Angstrom wavelength

exponent). A copy of a letter from Dr. Fraser acknowledging

receipt of these materials is presented in Appendix 'V,

Discussion

In this section, we will make some general observations

about the character of the data obtained during the

experiment. We will point out some of the interesting

features in the data, features that could reflect on either

the character of the aerosol or on instrument performaice.

-8-

T yy.JS .y, 9 . 

•n+r rtY .+. Tr .^*.^ _ _ _ ww. ,l'M.^S::
In perusing the data, we looked for: days that appeared

to have relatively constant turbidity; days when the

turbidity changed dramatically in a systematic manner;

sequences of days showing large changes in parameters.

The calculated values of alpha can be very sensitive to

relative changes in the measured aerosol optical depth or to

e trors in these measurements. Thus, a perusal of the alpha

values is often helpful in identifying trends or problems

with data points (or entire data sets). Assume for purposes

of illustration that we have error confined to one passband

in a pair of measurements in two different passbands - for

example, in the red channel of a series of measurements in

the red and seen. Then the error in alpha will be:

'a = A In r / 0.5653

The fractional error in the calculated alpha will be:

A 

a

Thus small errors in the measuredT

R

 will have an increased

impact at low aerosol optical depths and at low values of

alpha. This is illustrated in Table 3 which shows the

computed values of alpha (green-red) for induced errors of

+0.01 in the value of T R . Error alphas are computed for

various values of hypothetical "true" alpha and for various 

values of T R . For example, an error of ±0.01 for TR = 0.025 

will yield a range of alpha values of -0.5 to 1.0 for a

nominal "true" alpha of 0.1. An assumed error of 0.01 is

-9-
q

realistic. Of course, the problem would be compounded if

there were opposing errors of 0.01 in both channels. This

could explatn some of the trends in alpha observed at some

stations, especially on days with low aerosol optical deaths.

In the following sections we comment on each of the data

sets. In Table 4 we list the number of observations made

a

eacli day at each of the observing sites.

Goddard

We have previously commented on the excellent quality of

the Goddard data and the great abundance of data points.

Because of the large number of data paints, we are able to

discern more clearly any trends in the aerosol optical depth

values and also we are better able to reject anomalous data

points. On a number of days, the aerosol optical depths were

relatively constant and relatively lava : 7/11, 7/23, 7/30,

8/17, 8/18, 8/20, 8/23 and 9/9. On many of these days the

alpha values were relatively stable during the entire day and

they were relatively uniform across the spectrum.

However, on some days there were interesting variations 

in the alpha values. In some cases the alphas changed as the

day progressed and in other cases the value of alpha changed

across the spectrum. Interesting examples occurred on 8;/17,

8/18,, 8/20, 8/23 and 8/28. In most cases where alphas

changed across the spectrum, the alpha values were relatively

-10-
high in the blue/green channel, in the range of 1.5 to 2.5,

generally; in contrast, in the green/red, values were below l

and often ranged down to .5 and sometimes below. These

changes appear to be real and significant. Compare for

example, 7/30 with 8/23. In both cases the turbidities in

the red channel were approximately the same; the turbidities

in the green and the blue were progressively and

significantly different.

An interesting case worthy of further investigation is

that of 8/23. On this day, alphas were very low in the

blue/green channel, on the order of l or less; in contrast,

the alphas in the blue/red and the green/red were 1.5 or

higher. Despite the fact that some of the especially low

alphas in the blue/green occurred during low sun angles,

there seems to be a real change occurring in the properties 

of the aerosols during this day.

In conclusion, we can state that this data set is a very

impressive one indeed.

Philadelphia

This data set shows some trends which could be

attributable to real changes in aerosol character. On a

number of days the turbidity in the red channel was on the

order of .05 to .1; as the day progressed, the green/red

alpha values gradually dropped from about 1.5 to down to 0.5

V

I d

*, r

^t

-11-
-12-

or so. Examples are on 7/23, 8/18, 8/21, 9/23, 9/24, 9/25,

9/28, 9/29 and 10/27. The turbidity changes appear to take

place in the green channel. For example, on 9/24 the

turbidity in the red channel increases slightly during the

course of the morning from .061 to .072. In contrast, the

turbidity in the green channel drops from .143 and .185 to

.086. On 9/29 the turbidity in the red channel was .04 early

in the morning and was essentially the same value at 10:25;

however, in the green channel the turbidity drops from .092

to .037. The same sort of trend appears to be occurring to

some degree in the blue channel.

It is interesting to compare the Philadelphia data with

that of Goddard. Because they are located in the same

general region, we should expect some similarities. However,

the Philadelphia unit is located in the center of an urban

area whereas Goddard is rela • Gively rural. The first day when

there is data at both stations is July 18. On that day there

were two observations at Philadelphia and fourteen at

Goddard. At Goddard, the greens were about .5 and the reds

about .15/.16 in the mid morning. At Philadelphia, the

greens were .3/.4 and the red .13/.16. The green/red alpha

at Goddard was about 2.0 while at Philadelphia it was about

1.5/1.6. There was also data at these stations for the

succeeding 3 days. On the 19th at Goddard, the greens were

very consistent at about .63 to .60, reds were very
consistent at .20, and blues were about .95/.98. At

Philadelphia on July 19, turbidity values were a bit lower

than at Goddard; however, alpha values were similar.

Note that on 8/17 we have the first day at Goddard when

we see a significant: decrease in alpha in the green/red. A

corresponding change occurred tin Philadelphia on this day.

Similarly on 8/18 the alphas in the green/red decreased

markedly at Philadelpia and also at Goddard. This was

another day when turbidities were quite low at both

loco t.ions .

However, in general, low green-red alphas occurred

considerably more frequently at Philadelphia than at Goddard.

Because low alphas are caused by relatively higher concentrations of large particles, we could attribute these changes to

an increase in traffic-generated large particles as the day

progresses.

Rhode Island

This data set is not as extensive as some of the others.

There were problems with increasing amounts of cloud as the

experiment progressed. Also, because of the proximity to the

coast, fog was a problem. The instrument at Rhode Island,

No. 317, seems to have performed satisfactorily. Alpha

values appeared to be relatively uniform across the spectrum

on many days. However, on a number of occasions, the alpha

-13-
-14-

G

±t

t

t

^l values in the blue/green channel were often relatively high,

approximately 3 or greater. Some of these occasions were on

days when the turbdities were low. An example is on 7/30

and 7/31. Another example is the extensive series of

4r

;x measurements made on 8/17, 8/18, 8/20 and 8/21. The

F

turbidity in the red channel on these occasions was on the

order of .03 and .04 whereas those in the green were in the

general range of .5 to .6 or .7.

An extended period of low turbidities occurred at Rhode

Island and at Goddard beginning about 8/17 and extending

through about 8/23 on the Goddard record and 8/21 on the

Rhode Island record. During this period the data at both

stations appeared to be in reasonably good agreement in the

green and the red; however, the blues at Rhode Island

appeared to be a tittle on the high side. This resulted in

somewhat higher alphas involving the blue channel.

Nonetheless, the tendency for the alphas to decrease at the

higher end of the spectrum was evident at both stations. Low

green/red alphas occurred on a number of days during this

period. It was also during this time that low alphas in the

blue/green channel were noted during a several day period in

Philadelphia. Consequently, we conclude that during this

period the air mass conditions over the northeast in the

general area of the experiment were relatively homogeneous

and relatively clean.
Penn State

Two sun photometers were used at Penn State. Initially,

UM 314 was in place. However, towards the end of September

and into the beginning of October, there was evidence of

sporadic malfunctioning of the blue channel. When this

problem became evident, a second sun photometer, UM 311, was

sent to Penn State. Intercomparisons between the two

instruments were made at Penn State on October 11, 12, 18 and

19. For the most part the comparison between these two sets

of readings was quite good. Unfortunately, the weather was

poor during this period and Fn extensive series of readings

was not possible. There was also evidence of some

difficulties with cloud. During this intercomparison the

blue channel was essentially inoperative. However, the

difficultes with the blue channel apparently did not affect

the other two channels.

There is evidence that the blue channel in UM 314 began

to sporadically malfunction toward the beginning of the

experiment in July. This is evidenced by sporadic negative

values in turbidity and also unusually low, often negative,

values for the alphas involving the blue channel. However,

the turbidities measured in the green and the red channels

seem to be reasonably consistent even when the values in the

blue channel were wildly erratic.

-15-
On 10/17, turbidities were very low. There is some

evidence of a gradual change in the alpha G-R which may be

attributable to small but significant calibration errors

which become evident because of the very low turbidities. On

the whole, the alphas in the green/red are quite stable

during the course of the day during most of the data days.

This again suggests that the green and the red readings are

reasonably accurate and stable.

St. Louis,

The St. Louis data was taken with sun photometer No. U14

303. This is a very nice data set. There are a lot of data

points with many observations taken on most days when weather

permitted.

A perusal of the data shows that the data looks

internally consistent. Alphas are relatively constant across

the spectrum except on a few days. This is true even on some

days when the turbidities were relatively low - for example,

on days 7/20, 7/21, 7/30 and 7/31. However, there were no

days when the turbidity was consistently very Iow during the

course of the day. Conversely, on some days turbidities were

extremely high. On some of these occassions, blue/green

alphas were relatively low compared to the blue/red and the

green/red. An example is day 7/3.

The blue channel in this instrument seemed to perform

-16-
very well. On some days relatively constant blue turbidities

were obtained throughout extensive sets of readings during

the course of the morning. An example is on day 7/14. Day

8/5 is a bit unsual in that there were low alphas across the

entire spectrum. The next day the same situation obtained.

However, there was only two readings on 8/5 and one on 8/6.

Columbus, Ohio

This data set is a very nice and extensive one. The

data recovery was very good. There is data for many days and

on a large percentage of days the observer managed to take

the total prescribed set of readings, seven. There were a

number of days when the turbidities were relatively low and

constant. Examples are on 9/9 and on 9/23. On these days 

the alphas were relatively uniform during the course of the

measurements and they were essentially equal across the

spectrum. Typical values were in the range of 1.1 to 1.8 or

so. On a number of occasions the alphas in the blue/green

were unusually low with respect to those in the blue/red and

the green/red. Examples are on 7/6, 7/7, 7/8, 7/15, 7/23, 

8/4, 8/5, and 8/27. The turbidity on many of these days was

relatively high. Considering the fact that the alpha values

were essentially constant on many of the other days, these

days with low alphas in the blue/green are probably

significant - I.e., these are not instrumental artifacts.

-17-
.

The validity of the data which show low alphas in the

blue/green is further supported by comparing the Columbus

data with the St. Louis data. The first day on which data

was taken at both sites was on 7/7. On this day a similar

alpha trend was noted at both sites. On the following day,

7/8, the turbidities were extremely high at Columbus but they

were relatively low at St. Louis. In general, there was not

a great deal of agreement between these two data sets. The

turbidities, when they differed appreciably, were often

extremely high; this difference appears to reflect the

impact of local and regional pollutant sources. On 7/29 a

relatively clean air mass appeared to have moved into the

area and realtively low turbidities were noted at both sites.

This continued through 7/31 at St. Louis and into 8/1 at

Columbus. During this period St. Louis seemed to have

relatively higher alpha values than did Columbus. Another

period of relatively clean air began on 8/17 at Columbus and

8/18 at St. Louis. This persisted until about 8/20 or 8/21.

Some caution must be exercised in using the Columbus

data and, to a certain extent, the St. Louis data. Because

of the diligence of the observers, they often took

observations under marginal cloud conditions. Anomalous data

should be checked against the satellite photographs for

evidence of cloud contamination.
Conclusion

The sun photometer data obtained in this experiment are

probably the most extensive and coherent data set ever

obtained in experiment of this sort. Although there were

some instrumental dif-ficultias and although weather did

present a problem in the form of extensive periods of cloud,

in general the quality and quantity of data was quite

satisfactory.

-19-
f

Table 1

Sun Photometer Calibration Constants For Three Calibration Periods

Ina t Calib Slue Green Red Water* Notes

Uh1302 1 TT-.9 217.6 169.2 =.1 2

2 39.5 216.4 170.4 -

3 42.2 217.1 169.2 1.84

UM303 1 70.6 227.6 173.5 1.76

2 67.4 222.6 172.3 -

3 68.7 225.6 169.3 1.79

UM310 1 - - -

g - Instrument Malfunction

During Test

2 50.9 217.6 193.4 -

3 52.5 217.1 189.5 1.83

UM311 1 62.3 234.3 146.4 2.38

2 65.6 237.5 147.9 -

3 68.2 242.7 152.1 2.37

UM314 1 - - - - Not Run

2 27.8 177.1 159.3 - 

3 27.1 182.5 160.1 -

UM315 1 4318 206.3 182.2 1.74

2 46.2 209.4 186.7 -

3 49.1 209.9 188.9 1.63 

UM317 1 47.2 205.0 175.9 1.73 

2 44.7 202.6 174.5 - 

3 47.5 200.6 172.0 1.65

UM319 1 - - - - Not Run

2 46.0 181.6 149.5 2.15

3 47.7 180.0 149.5 2.10 

UM320 1 30.0 - 141.1 -

2 29.0 186.3 140.1

3 29.6 185.1 142.3 2.08

UM322 1 32.1 185.5 150.9 1.90 Prime Langley

Calibration

2 Reference Instrument for this Calibration

3 36.3 190.8 151.0 1.83

UM323 1 39.2 182.5 125.7 2.06

2 - - - - Not Run

3 39.1 184.3 125.8 2.03 Prime Langley Calib

(Boulder)

+Calibration Period

40 

-20-

__

. ..:..j., ^_. ....
i

Table 2

Recommended Sun Photometer Calibration Constants

k

Inst. Blue Green. Red Water

UM302 40.9 216.8 169.8 1.84

UM303 68.1 224.,1 170.8 1.79

UM310 51.7 217.4 191.5 1.83

UM311 66.9 240.1 150.0 2.37

UM314 27.5 179.8 159.7 -

F

UM315 47.7 209.7 187.8

1.63

U;,317 46.1 201.6 173.3 1.65

UM319 46.9 180.8 149.5 2.13

UM320 29.3 185.7 141.2 2.08

UM322 36.3 190.8 151.0 1.83

UM323 39.1 184.3 125.8 2.03

Simple mean of constants from calibration periods

2 and 3 exc-apt for UM322 and UM323 which are

simply the values from calibration period 3.

Water channel constants for all instruments are

i^ from the third calibration period only.

j

L.

y i.
f

e

4X

Y

f Table 3

Error Sensitivity in Alpha. Effect on Alpha of an Error

of 0.01 in T R with T G Constant

Nominal Value of (G - R)

^ TR 0.1 0.5 1.0 1.5

Error Ranee in Alpha

0.025 —.500/1.00 —.100/1.40 .400/1.90 :90012.=o

0.05 -.233/.495 -.177/.895 .677/1.40 1.18/1.90

0.10 -.069/.286 .331/.686 .831/1.19 1.33/1.69

0.50 .065/1.04 .465/.504 .965/1.04 1.47/1.50

-22-
Table 4

Number of Observations Per Day at Each Station

July

S^ . Teo. Colo. P.S. Phila. R.T. God

1

2 2 1

3 5

4

5

6 5 1 2 7

7 7 6 6 23

8 6 7 5 6

9 6 4 4 4 29

10 1 1 4 5 14

11 7 6 4 1 26

12 4 1 3 12

1.3 3

14 7 6 3 1

15 3 6 5 6 14

16 2 5

17 7 7 6 6 5

18 2 5 5 2 14

19 1 3 6

20 7 

21 7 4 17

22 7 1 2 2

23 7 .3 5 16

24 5 6 3

25 3 7

26 2

27 1 1 3

28 1

29 5 2 3

30 6 7 4 3 22

31 7 7 7 2 5

-23-
L

Table 4 (Conb'd)

August

1

2

727

2

1

57

3

1

3

4

7

3

5

2

5 .3

1 19

6

11

7

4

1

8

6

9

78

10

4

1

3

11

3

1

12

7

5

13

52

14

2

2

3

1 15

15

1

16

4

17

3

7

4

2

5 20

18

78

74

5 16

19

7

2

20

3

7

7

2

3

9

21

5

1

5

3

7

22

1

23

3

4 19 

24

2

3

1

25

4

2

3 14

26

5

27

3

2 

28 16

29 

30

31

2 • 

-24-
Table 4 (Cont'd)

September

1 4 1

2 5

3

4

5 a

6

7

8 2 2

9 7 1 18

10 4 2 2

11 7 1/1 2

12 6 2/2

13

14 4

15 End 

16 2 1

17 1

18 2 2/2

19 4 2/2

20 1

21 2 4

22

23 2 5 6 

24 4 /1 5

25

26

27 1 

28 2 5 1 2

29 3 1 1 4

30 2

31

-25-
-26-

Table 4 (Cont'd)

October

1 1

2 2

3

4

5 2

6

7 1 2

8 2 4

9 1 3

10 End

11

12 6 1

13 3 3

14 2 5 3

15 End 1

16 2

17 5 2

18

19 2

20 2 2

21 End 2

22 End

2

End
v

Appendix I

Sun Photometer Measurements

Instructions to Observers
E,

x

SUN PHOTOMETER MEASUREMENTS

NORTHEAST TURBIDITY (NET/91)

Dr. J.M. Prospero and Mr. T. Snowdon

University of Miami,

Rosenstiel School of Marine and Atmospheric Science

4600 Rickenbacker Causeway

Miami, Florida 33149

Telephone: Prospero.-305/350-7440

Snowdon-305/350-7464

R

z... 

lei

i
► r 

r

PURPOSE

The measurement of the intensity of direct solar radiation in narrow

wavelength bands enables us to determine the amount of aerosol extinction

(turbidity) and the spectral dependency thereof. The measurements which you

make will provide ground truth for a satellite program which endeavors to develop

techniques for the remote sensing of pollutant aerosol concentrations.

INSTRUMENT

The sun photometer is similar to a photographic exposure meter with a very

narrow viewing angle. Your instrument measures at four wavelengths: 1) 380 nm,

which we will refer to as the blue (B) wavelength; 2) 500 nm, which we will refer to

as the green (G) wavelength; 3) 875 nm, which we will call the red (R) wavelength;

4) 945 nm, a water vapor wavelength (W). The instrument is also used to measure

the relative optical path length, or air mass, (M).

The instrument functions as follows: Filters are mounted on a disc that is

rotated by the large knob at the rear of the box. The filter can be, viewed through

the glass cover plate at the front of the box by removing the snout cover. The

readout device is a liquid crystal display (LCD). With the Function knob on the top

of the case placed in the PreAmp (PA) position, the amplified voltage output of the

silicon detector is read by the LCD voltmeter. With the knob placed in the Peak

Hold (PH) position, an electronic circuit is incorporated which records and holds the

maximum reading obtained. The third position, Thermistor (T) yields an analog (not

true) temperature reading of the silicon detector; the reading increases with

decreasing temperature. In routine operation, only the Peak Hold and Thermistor

functions will be used.

The diopter arm along the side of the case is used to measure the solar

elevation in terms of the relative path length through the atmosphere M. At solar

noon, M=1 and it increases with increasing angle from the zenith.

MAKING MEASUREMENTS WITH THE SUN PHOTOMETER

A) Turn on the instrument as soon as you pick up the instrument to walk to the

observing site. Carry the instrument with the strap around your neck or use

the carrying case -if one is supplied; do not use the neck strap as a hand

carrier - there is danger that the swinging instrument might strike something.

B) Pick a site that is relatively protected from the wind if possible.

C) Time. Immediately prior to making a solar reading, note the Local Daylight

Saving Time to the nearest minute. Use the watch on the photometer; it is

set to your local daylight saving time.

D) Temperature Reading. Place the Function switch in the Thermistor position

and record the LCD reading on the data sheet. (This is not a true

temperature).
e _,

t ` , E) Solar Reading. Function switch In Peak Hold position:

1) With the Filter knob in the Blue position, momentarily press the Reset

button and then aim the Instrument at the sun so that the sun spot falls

on the target. It Is not necessary to have the spot precisely on the

target; instead, sweep the spot repeatedly across the target until the

LCD reading is stable. (In practice, the last digit may wander up or

down a few units - this Is acceptable). This sweeping action should take

only several seconds. Note the reading; Reset and repeat the procedure

u to verify the reading. Always Reset the instrument when it is pointed

at a relatively dark part of the sky or at the ground. It will not Reset

properly to zero when pointed at the sun.

a) Switch to Green and repeat the sequence.

b) Switchto Red and repeat the sequence.

c) Switch to W and repeat.

^- 2) Note the time. I

3) Set the Function switch to Thermistor and note the reading.

' 4) Return the Function switch to Peal< Hold and repeat the entire

sequence.

a) Time

b) Thermistor

c) Blue readings

d) Green readings

e) Red readings

f) "W" reading

g) Solar elevation reading M. The value of the relative optical path

length (M) is read at the point where the top of the case intersects

the diopter scale-see figure. (M is a measure of the optical path

length through the atmosphere. When the stu n is directly

overhead, M=1. An M value of 3, for example, indicates a path

length through the atmosphere that is 3 times that with the sun

overhead).

h) Time

1) Thermistor reading

t The second set of readings should be within several percent of the first set.

If not, thin high cirrus may have been present or the readings may not have been

made carefully. To check the latter possibility, repeat the reading sequence.

If you have notes or comments, write them out on the line immediately under

the data line.

Time readings must be accurate to within one minute.

F) At the completion of the readings, turn the instrument to Peak Hold and OFF

and return it to its storage place.

G) Record all data on the forms which we supply. Always make a carbon copy.

Mail each week's supply of data to us on Friday evenings. Send the original.

Keep the carbons until the end of the experiment when you can mail there as

a batch.
We encourage you to have some patience during the first few days of using

this Instrument. After a little experience, the measurements will not take more

than several minutes.

WHEN TO MAKE READINGS

Readings will be made only during the morning hours up to about solar noon.

There Is a tendency for cloud to build up later in the day; this makes satellite data

interpretation difficult. Hence, we will not ask for afternoon readings.

Your schedule calls for a series of four prime readings spaced throughout the 

morning. You will be reimbursed for these readings. You also have the option of

taking as many as three additional measurements for which you will also be

,reimbursed, but at a lesser rate. The rationale for selecting these times will be

more obvious if you refer to the appended figure which shows the value of M (the

relative atmospheric optical depth) as a function of time on selected dates at your

location. The first measurement is scheduled for 7:00 a.m. or earlier (see appended

diagram). This time yields a relatively high value for M; also, convection should be

minimal at this hour. The second, third and fourth prime measurement time slots

are progressively longer because the rate of change of M is progressively slower. In

recording the time of measurements in the early hours, it is necessary to be

accurate to within + 1 minute because of the rapid change in M. Although we will

use your measured value of M in the computer computations, we will also calculate

the value of M for verification purposes.

The Additional Measurements A, B and C are Interspersed between the Prime

Measurements. Note that you must allow a gap of about 15 minutes or more

between the Prime Measurements #1, #2 and #3 and the Additional Measurements

A and B. Measurement C must be separated by at least 30 minutes from #3 and #4.

The objective is to get a set of measurements that are relatively uniformly

distributed throughout the morning.

The gratuity scale is as follows:

#1 = $1.75

#2, 3, 4 = $1.25 each

#A = $0.75

#B, C = $0.50 each.

Also, the person making the greatest number of useful readings will receive a 

bonus of $100. Those -in second and third place will receive $50 and $25,

respectively. Thus, a person making prime measurements every day during July and

August will receive a total of $341. If all possible additional measurements are 

also made, the total will be $450. There is also the added possibility that you might

win a bonus. Remember, however, that only valid measurements will be

reimbursed. Measurements made through cirrus or in areas of heavy cloud (both of

which are discernable in our satellite imaging) are obviously invalid.

WHERE TO MAKE READINGS 

You may make readings anywhere within the general area of the town or city

specified in your address. For example, you can make the early morning readings

^i

NO
at your home and the later readings at your lab. However, if you make readings at

locations other than the laboratory address, please give us the precise address of

such locations the first time you take readings at that location. Thereafter enter a

brief note in the Notes column as to the location (i.e., home, lab, etc.). Always

carry the instrument in the carrying case provided. Do not let the case stand In the

sun for long periods.

Do not make readings when there is cirrus over the sun or when clouds are

over or within a few degrees of the sun.

COMMENTS ON TURBIDITY MEASUREMENT TECHNIQUES:

Always record the maximum reading; the maximum reading will not

necessarily be obtained with the aiming spot directly on the target.

The Blue channel readings will always be much lower than those in the Red,

Green, and' V" channels.

Occasionally check the glass plate covering the aperture at the front of the

instrument, take off the snout aperture and look down the tube. If it is dirty,

remove the snout and wipe very carefully with optical tissue.

If you take the instrument from an air conditioned room to a hot, humid

environment, condensation may develop on the glass cover plate. It is best to store

the instrument at a temperature that is not too different from that of the outside

air.

Do not let the instrument sit in the sunlight for long periods of time - it can

get quite hot and affect the calibration.

The instrument does not like being dropped. If it is dropped, make a note in

the log sheet so that we will be alerted to possible changes in instrument

characteristics.

You may find that the last digit on the LCD display has a tendency to wander.

This i^ especially true for the blue channel which has a very high gain. A wander of

a few tenths (i.e., in the last digit to the right) is not significant. However, if the

wander approaches one digit in the units column, make a note in the data sheet and

inform us by telephone.

Please call either Prospero or Snowdon if you encounter any problems. We

will have several spare instruments on hand to replace any faulty units.

About once a week, make a check of the sun photometer watch against an

accurate time source. Record the clock time (hours; minutes; seconds) the instant

that the watch minute readout changes. It is not necessary to reset the watch

time. The watch is set for Local Daylight Saving Time. The watch has a readout

of month and day which is activated by pressing the button on the side once.

-s - -

_.... .-
BATTERY CHECK AND REPLACEMENTS

UM SERIES - 300 Sun Photometers with 4 filters contain three (3) 9v batteries (see

wiring diagram):

1. Battery #1 powers the peak hold and temperature circuits as well as providing

positive voltage for the photo-detector/amplifier. This battery provides more

current, 7-l0 ma in the temperature mode, than the other two batteries.

Test Jack #1 provides access to Battery I and must be read with the

photometer ON and in either the PEAK HOLD or PREAMP mode (i.e., not in

the Temperature mode).

.^

2. Battery #2 provides negative voltage for the photo detector/amplifier

(B&H529). Only 0.4 ma are drawn form this battery, so It should last

indefinitely under normal use. Test Jack #2 accesses this battery.

3. Battery #3 provides power to the voltmeter board and the digital display.

This battery only needs to deliver 1.2 ma; it too should last many months in

routine service.

The battery test need only be made every few weeks unless there is a

possibility that the instrument has been left ON for an extended period of time

(more than a few hours).

Checkin g the Batteries: Test Pin Jacks are provided. for batteries 1 and 2.

1. Place instrument ON and in PEAK HOLD or PREAMP position. 

2. Connect the positive lead of a voltmeter to the appropriate pin jack and the 

negative lead to the large strap screw-head next to jacks.

3. Voltmeter should read in the range of 7.0 to 9.1v. If the battery yields less

than 7.0v, it must be replaced.

4. There is no test jack for battery #3 (voltmeter board). A weak battery is

Indicated by a feeble display.

Battery Replacement:

1. Unscrew four rubber feet and remove bottom plate from instrument.

2. Remove Styrofoam wedge and lift out batteries.

3. Batteries can be easily identified by checking the destination of the black

lead from the battery clip.

a. Blacklead to outer (light green) circuit board on right - Battery 1.

b. Black lead to dark green integrated circuit socket on left - Battery 2.

C. Black lead to inner (dark blue) voltmeter circuit board on right -

Battery 3.

s ;
4. If any one batterX is weak, replace all batteries.

5. Ba,cterles should be replaced with fresh 9v alkaline transistor batteries

(MN1604 2 V51323p or equivalent). We will reimburse you for the cost of

replacement batteries if you send a receipt for their purchase.

G. Always turn off the Instrument when replacing the batteries.
7 & '—1 /0 13 /0

19MIllimetcra to the Ccotluitur

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Appendix II

Observation Stations and Observers

............. . . .
Appendix II

Observation Stations and Observers

Philadelphia Terry Bandy - Drexel Univ. 75:1OW 40:OON

Bryn Mahr 75:26W 39:95N

Ruth A1ee - Drexel Univ. 75:1OW 40:OON

Home Same

NASA/Godadard Wang - GSFC 77:OOW 38:92N

Fraser - Kimberly Rd.

or

Fredrick (Md. ?)

or

Washington Pk.

URI R. Cayer - Narragansett, RI 71:45W 41:43N

St. Louis J. Hulka - Washington Univ. 90:25W 38:67N

PSU D. Kabel - St. College, Pa. 78:54W 41:11N

Clearfield, Pa. 79:23W 41^02N

(7/11/81 only)

M. Nichols - St. College, Pa. 78:54W 41:11N

(began 9/11/81)

Centre Hall, Pa. 77:58W 40:92N 

OSU W. Stockwell - Columbus, Ohio 83:05W 39:98N
Appendix III

Cover Letter to Observers
Universityi of Miami Miami, Roda 33149

DIVISION OF WAINE GEOLOGY FIND GEOPHYSICS

Dorothy H and Lewis Ilosenstic.-I

School of Morino and atmospheric Science

4600 Rickenbocker Causeway (305) 350,7508

June 22, 1981

a

Dear Colleague:

First, we wish to thank you for agreeing to cooperate in this

experiment. The objective of our program is to use remote sensing

techniques to measure the vertically integrated aerosol concentrations

in pollution episodes. Dr. Robert Fraser (NASA/Goddard) will use various satellites, principally the geostationary satellite (GOES) and

the Coastal Zone Color Scanner (which actually scans well inland), tin

measure surface brightness values which can be inverted to yield aerosol

optical depth estimates. The sun photometers which we are placing in

the field will provide ground truth measurements which Dr. Fraser will

subsequently fold into his inversion model.

The sun photometer is fully described in the appended literature.

Briefly, it is a device for measuring the direct solar radiation intensity in relatively narrow passbands (380 nm, 500 nm, 875 nm, and 940 nm).

The presence of aerosols will result in a reduction of the direct; solar

radiation through the atmosphere because of scattering and/or absorption

by particles in the optical path.

The measurement protocol is fully described in the instructions.

Briefly,we are asking you to make measurements during specified time

periods during the morning during July and August. You will be paid

for each measurement that you make. There are four prime measurements.

You will be paid $1.25 for each of these except the first for which you

will receive $1.75 (because it is relatively early in the morning). Note

that the allowable time slot broadens as the morning progresses. This

is so because the rate of change of the light path through the atmosphere

is greatest at low sun angles. You may take additional readings at times

other than the prime time slots as shown in the schedule; you will be paid

$0.75 for the first reading and $0.50 for the others up to a maximum of 

$1.75 per day. There will be a bonus of $100.00 for the person who takes

the greatest quantity of valid data during July any.' August, a bonus of

$50.00 for the person who takes the second greatest quantity of data, and

$25.00 for the third greatest. Payment will only be made for valid data

including both Prime Measurements and Additional Measurements. There will

be a total of five paid observer stations in the network.

' d Prhrnfd 6-4,mncx^f intarnnhnnnl I lnivarmh i An Fn+ inl C7nnnrh inih i / Affirmntiv p Artinn Fmnlni iAr 
Page Two

We will be analyzing all satellite data for the months of July and

August including weekends. Thus sun photometer data for weekends will

be utilized. We encourage you to make weekend measurements.

The instrument is so easy to use that you may want to teach more than

one person to use it and to make readings. However, you must be careful

that, in assigning more than one person to make readings, the readings

don't get taken because person A thought B was doing it while B thought

otherwise.

n

We will be most happy to supply all interested parties with aerosol

optical depth values once we have complet,ed the computations. Note that

one channel (940 nm) will give us a measure of precipitable water, a

number which may be of interest to some of you.

We will ship all instruments this week. We hope that you will immediately begin to use your instrument so that you will get a feel for

the instrument and verify that it has not been damaged in shipment. If

you have any difficultieo or questions, please call us collect. We have

several spare photometers with which we can replace malfunctioning units.

One of us (J.M.P.) will be away from 27 June until 28 July, but the other

(T.S.) will be here at all times. The telephone numbers are: Joe Prospero,

305/350-7440; Tom Snowdon, 305/350-7464.

Please return data sheets by mail each Friday night at the end of

operations. This enables us to check the data for internal consistency.

A supply of self-addressed stamped envelopes are enclosed with the photometer.

Please advise us as soon as possible of telephone numbers where you

can be reached while in the field.

Thank you and good luck.

C::9osVeph M. Prospero

Sincerely,

^' ` '^lWv v _y

Professor

Marine Geology and Geophysics

Thomas Snowdon .

Research Assistant

JMP/mh

}

a
^

^

_

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e

Appendix I\7

Standard Data Form
II i caS.

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Appendix V

Letter Confirming Receipt of Data:

R. Fraser
National Aeronautics and

Space Administration

Goddard Space Flight Center

Greenbelt, Maryland

20771

NASA

Reply to Altn of

915 FILE 14139

Professor Joseph M. Prospero

Division of Marine and Atmospheric Chemistry JUL 14

4600 Rickenbacker Causeway

University of Miami

Miami, FL 33149

x. Dear Joe:

I have received from you the solar transmission data taken during the

summer and fall of 1981 under Contract NAS5-26768. These data are

given on IBM cards and are listed on tabulations. I shall return

your 3 transmissometers to you at the end of this month.

Sincerely,

Robert S. Fraser

Climate and Radiation Branch

Laboratory for Atmospheric Sciences
REPORT OF INVENTIONS AND SUBCONTRACrS I FORM APPROVED 

(Pur~uant to "Patent Rights" Contract Clause) (See Instructions on Reverse Side) O.'rfBNO. 22-R160 - t. NAME AND ADDRESS OF CONTRACTOR (Include Zip Code) 2. CONTRACT NUMBER 

. Joseph M. Prospero, Dennis Savoie, Thomas Snowdon and Paul Ewbank NASS-26768 

University of Miami, Rosenstiel School of Marine and Atmospheric Science 3. TYPE OF REPORT (Check One) 

4600 Rickenbacker Causeway, Miami, Fl 33149 l"Ia. INTERIM f"Xi b. FINAL 

SECTION I - INVENTIONS ("Sui!Jject Inventions") 

4. INVENTION OAT A (Listed below are all inventions requirt'!d to be reported) (11 uNone." sO tirate) 

(i) (ii) (iii) CONTRACTOR (i"JCONTRACTOR (,,)C~I~~~~ ~~RY 

OISCLOSURE E!..ECTS TO ASSIGNMENT 

FILE U. S. FORWAROED TO NAME OF I .... VENTOR(S' TITLE OF INVENTlON IOENTIFICATION -';UMBER PATENT CONTRACTINC OR PATENT APPLICATION APPLICATION OFFICER 

SERIAL NUMBER YES NO YES NO 

00 

.-n ?2 

NONE -oG) 

02 

0"" :01"'" 

.0-0 

C~ 

J:;>~ 

r-ffl 

~e1 , 

... SECTION" - SUBCONTRACTS..1ContaininR D "Patent R;Shts" Cla,,:;e) 

S. SUBCONTRACT OATA (Lr~rC'd;s information required LuI not previously reported lor SubcontraC"t:!!-JJ!f ·-NOl1«-· .. !'tO stat~ 

(i) NAME AND ADORESS (ii) (ii,) SUSCONTRAC T (iv) (VI SUBCONTRACT CATES 

OF SUBCONTRACTOR SUBCONTRACT PATFNT R.C .... TS wORK TO BE PERF'ORMED UNOER SUBCONTRACT 

(Includ~ Zip Code) NUMBER .. CLAUSE AWA.RD COM"!.. E nON 

. NONE 

- J 

SECTION III - CERTIFICATION 

CONTRACrOa CERTIFIES THAT PROM?T IDENTIFICATION AND TlMEL Y DISCLOSURE OF SUBJECT INVENTIONS PROCEDURES HI'.""JE BEEIII FOLLOW EO 

DATE NAME AND TITLE OF AUTHORIZED OFFICIA!. (Pri,., ur Tn"') SIG ~ATURE 

7/21/83 Joseph M. Prospero, Professor o~M ~YJI., _ ... /1 Tl 

·1 FORM 882 SIN 0102-lF~~820 \ J 1 , EDITION OF t JUL 68 IS OBSOLETE f OCT 7!1 

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