text: Last Thursday William Schambra, director of the Bradley Center for Philanthropy and Civic Renewal, introduced a panel of speakers to address the question "Is Philanthropy a Profession? Should It Be?" (Scott Walter previewed the program earlier on this blog.) Schambra asked whether philanthropy is, or should aspire to become, a body of rational knowledge worthy of scholarly specialization and the awarding of academic credentials. Can it ever achieve measurable levels of certainty and teach methodologies for replicating and diffusing knowledge? Or is philanthropy a kind of liberal arts "wisdom" based on lived experience and roughly fashioned by trial-and-error? The latter opinion was the view of the principal speaker, Karl Stauber, president of the Danville (Va.) Regional Foundation, whose summary of his published paper in the Foundation Review kicked off the discussion. Stauber's article, "Philanthropy: Are We a Profession? Should We Be?" raised more questions than it answered, but concluded "[M]y fear is that the 'scientific' approach most often drives us to focus on what is easiest to measure, which is not the same thing as what is most important." Unlike doctors and medical schools, which accumulate and disseminate ever-more precise bodies of knowledge, Stauber noted that practitioners of foundation philanthropy have few theories of knowledge or standards of measurement. Their achievement, said Stauber, typically consists of the finding the "right" people with "vision" and "principle" and "commitment," concepts notably lacking in rigor and clarity but essential to successful philanthropy. While successful philanthropic programs and projects can be shared with others, there is no telling whether the results can be repeated. The reasons for a grant's success or failure are indeterminate, conclusive one time, inconclusive the next. Stauber remained upbeat about the potential of philanthropy. As a practicing philanthropist, how could he not be? But can philanthropy become a profession? No. Three persons responded to Stauber's presentation: Teri Behrens, the editor of the aforementioned Foundation Review (which identifies itself on its front cover as "the peer-reviewed journal of philanthropy"); Joseph Paulus, who is getting a Ph.D. from the Indiana University Center on Philanthropy; and Susan Wolf Ditkoff, a partner at the Bridgespan Group, a management consulting and executive search firm spun-off from Bain & Company. Bridgespan assists nonprofits that want to learn how to "recruit leaders," "manage performance," "fund our mission," "develop a strategy," and "build our organization." It's fair to say that overall the three respondents took the pro-profession position. They argued that philanthropic expertise is needed. You have to be able to evaluate funding proposals regarding the provision of health, housing, education, you name it, and the more complex the need, the greater the demand for philanthropic expertise. A practitioner of foundation philanthropy—I gather the term "grantmaker" is now considered vulgar and inappropriate—needs real knowledge about the capacity of funding proposals to achieve their objectives and whether grant recipients are able to innovate to respond to new needs and changing conditions. This requires knowing how to "do" philanthropy well and how to do it better, which implies that philanthropy must become a profession: Philanthropists need to have specialized knowledge; they must develop techniques for sharing what they know and create methods for training others who would understand and apply what is known (and give them the credentials that acknowledge their authority). No wonder you need to go to grad school. The advocates admitted that there are pitfalls on the road to professionalization—mistaken ideas and exaggerated expectations. Ditkoff pointed to the ignorant venture philanthropist who wants to create a "Morningstar for nonprofits" to evaluate 501(c)3s. Then there is the compulsive process-oriented grantmaker who in return for a nominal sum expects harried and over-stretched charities to submit lengthy applications and post-grant evaluations to ensure due diligence. Ditkoff's advice: If a grant applicant is engaged in disaster relief, "just give them the money." Nonetheless, she argued that donors need to know how much time and money and expertise is needed for grantees to solve problems and maximize returns, and this speaks to the need for becoming professional. Stauber had suggested that philanthropy may lose sight of what is important if it focuses on data and the fad of measuring "effectiveness." But Schambra offered some concluding criticisms of professionalized philanthropy that cut more deeply. As he has frequently observed, advocates of philanthropic professionalism favor systemic "root cause" explanations of social problems, and they often disparage "band-aid" approaches to giving. Those who consider themselves most progressive support so-called "social change philanthropy," a funding strategy that requires more than producing better metrics to evaluate educational achievement or healthcare quality. It requires giving money to support community organizing, social activism and political advocacy. But this type of grantmaking affects power and values, matters that are never measured like improvements in reading scores. Foundation leaders look enviously at social science professionals who invoke their claims to expertise to influence politicians and judges. Is it any wonder that they envision a comparable influence for themselves, one in which entering the magic circle of "peer-reviewed" scholarship will give them a similar cachet?


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Home Chevron icon It indicates an expandable section or menu, or sometimes previous / next navigation options. Culture
YouTube stars were kicked off a Caribbean cruise after a single night for wreaking havoc with lewd pranks, according to their latest video
Ellie Abraham
The NELK Boys were told to disembark the ship after just 20 hours.
Buena Vista Images/Getty
YouTube collective NELK Boys were ordered to disembark a cruise ship after a day on board.
In a video documenting the events, they appear to make lewd comments and pull pranks.
In the video, they said their intention was to "fuck with some people" and get kicked off the cruise.
A group of YouTubers from the Canadian content collective NELK Boys were removed from a four-night Caribbean cruise to the Bahamas after just one night on the ship, according to their latest YouTube video.
The 25-minute video was posted Tuesday and has been viewed over 3 million times at the time of writing. It is titled "We Got Kicked Off a Cruise!" and includes footage that purportedly shows the group asking staff crude questions and heckling a show, among other disruptive incidents, with the apparent intention of being removed from the cruise.
Representatives for the NELK Boys did not immediately respond to Insider's request for comment.
"We're the only people to book a five-day cruise with the intention of getting kicked off. We were there for one day," said NELK member Stephen Deleonardis in the video.
While waiting to board the ship — which, according to logos visible in the video, appears to be operated by Celebrity Cruises — in Miami, the video shows NELK cofounder Kyle Forgeard asking a staff member if there are drugs in the water. When contacted by Insider, Celebrity Cruises declined to comment on the contents of the footage.
Later in the video, Deleonardis was filmed asking a person who appeared to be a member of housekeeping staff providing hot towels whether they were "jizz rags," and went on to ask someone else who appeared to be a staff member whether they could book "tuggies," a slang term for masturbation. At a later point, the group can be seen taking lewd photos by a Christmas tree.
During another scene, a woman can be seen in the background asking someone to help because "they're not turning their cameras off." The group then appears to be approached by a staff member who tells them the woman felt "insulted" by their behavior.
The video later shows the group attending an event featuring a speech from the captain and a comedy show, during which NELK member Salim Sirur can be seen heckling, while other passengers tell him to "shut the hell up." The footage then appears to show security guards removing him from the room to applause from fellow guests.
A woman who identified herself as the cruise ship's security supervisor was then filmed telling Sirur and Forgeard she was wearing a body camera and she would share the footage with law enforcement.
"Whatever you're doing, your behavior is not allowed on board," she can be heard saying, before warning them they may have to leave the ship if they continue.
The following day, Sirur and Forgeard were filmed being asked to meet with the hotel director. They were asked not to film, but appeared to capture audio of them being reprimanded for using coarse language and disturbing guests.
According to on-screen text shown during NELK's video, the group was "advised to disembark" the ship within the next 15 minutes. Elsewhere in the video, Forgeard said the goal of the trip was to "fuck with some people."
"This is an older crowd, this whole cruise. So, we're going to really try to take advantage of the pranks and fuck with some people. Just troll them and shit," Forgeard said.
The NELK Boys have been posting YouTube videos since 2010 and now have 7.17 million subscribers and a combined total of over 1.1 billion views. Their videos typically show them pulling pranks on members of the public, and feature crude humor.
In September 2020, the channel was demonetized by YouTube after the members encouraged fans to flout COVID-19 guidelines by promoting a party at Illinois State University, The New York Times reported. Footage posted on Forgeard's Instagram story at the time showed that a large gathering took place.
"We suspended the NELK channel from the Partner Program because they encouraged large numbers of people to disregard social distancing guidelines, creating a large public health risk," YouTube wrote on Twitter.
For more stories like this, check out coverage from Insider's Digital Culture team here.
More: YouTube Influencer Cruise Digital Culture

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ITG steht für:

 IT-Governance, Element der Unternehmensführung gewährleistet, dass die IT die Unternehmensstrategie und -ziele unterstützt; Ursprung US-Administration; siehe auch CGEIT certification.
 Informationstechnische Grundbildung, Unterrichtsfach in Deutschland
 Ignaz-Taschner-Gymnasium, nach dem Künstler Ignaz Taschner benanntes Gymnasium in Dachau bei München
 in Baden-Württemberg: Bezeichnung für ein Technisches Gymnasium mit dem Profilfach Informationstechnik
 Informationstechnisches Gymnasium
 Informationstechnische Gesellschaft, Fachgesellschaft im Verband der Elektrotechnik, Elektronik und Informationstechnik e.V. (VDE)
 Internet telephony gateway, ein Internet-Telefon Gateway wie z. B. das LevelOne VOI-8000, mit denen analoge Telefone digitalisiert werden können.
 In The Groove, ein Videospiel
 International Trumpet Guild, 1975 gegründete weltweite Organisation von Trompetern
 ITG Brands, drittgrößter Tabakwarenhersteller der USA

ITG

redpajama_set_name: RedPajamaWikipedia


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text:
The Crowd at the Foot of the Cross
The Crucifixion, 1538 by Lucas Cranach the Elder
Sermon preached at Church of St. Paul and the Redeemer, Chicago
Roger Ferlo
This year at this Good Friday service, we are introducing a new practice to complement our much more ancient one.
The ancient practice will be familiar if you have come to this service before. In a few moments, we will bring a large, rough wooden cross into the room, in solemn procession down this aisle. As soon as the cross is in place, the Prayer Book informs us in a carefully worded rubric that "appropriate devotions may follow." That's implicit permission for us post-Reformation Christians to revive a pre-reformation Good Friday ritual. Once we've set it down, everyone here should feel free to approach the foot of the cross in an act of veneration. Some of us might simply kneel there for a moment, in silent contemplation. Some of us might reach out to touch the wood. Some might even kiss it. If past experience holds, a number of us will simply remain in our places, sitting still and silent, perhaps a bit uneasy, absorbed in our own private reflections. Whatever you decide is appropriate. Meanwhile, the choir will sing settings of one of the few anthem texts included verbatim in the Prayer Book itself:
Savior of the world,
Who by thy cross and precious blood hath redeemed us:
Save us and help us, we humbly beseech thee, O Lord.
That's the ancient practice. But if you've attended Sunday services here during Lent, you would have heard that we are also starting a new one. You would have had an opportunity to write a prayer or intention on a little card, seal it in an envelope, and deposit it in the empty baptismal font. As we carry in the cross today, we will carry in all the cards that have been collected in the past few weeks. We will strew them at the foot of the cross, as silent testimonies to our sorrows, penitence, cares, and desires, both for ourselves and for those who matter most to us.
It will get crowded today at the foot of the cross.
If we can believe the Gospel accounts, that would not be unusual. There were quite a few people gathered on the killing ground outside the city gates to watch the original proceedings. I did a quick census of the four gospels. Mark and Matthew set the record for attendance. Besides the soldiers; the chief priests and scribes; those who passed by; and the bystanders, Matthew and Mark single out as many as nine people specifically, several of them by name: Simon of Cyrene; the two bandits; the centurion; Mary Magdalene; Mary the mother of James and Joseph; the mother of the sons of Zebedee; Salome. In his gospel, Luke talks about the "great number of people" who followed Jesus to watch the "spectacle." "Spectacle": that's Luke's word, not mine. Witnesses to the spectacle, Luke says, besides the soldiers and the rest, included all Jesus' acquaintances, including the women who had followed him from Galilee. They perhaps wisely stood at a distance, but close enough to see. Then of course there was Joseph of Arimathea, who helped get the body down from the cross once the crowd dispersed. John's gospel also mentions Nicodemus. He's the one who John tells us had come to Jesus in the middle of the night, who was told to his dismay that he needed to be born again, born from above. Who knows what was going through his mind if he remembered that encounter as he helped Joseph wrestle down the corpse. John's account also mentions a crowd, but like a good cinematographer John likes to engineer dramatic close-ups. The crowds disappear as the camera zooms in on Jesus' mother and the disciple whom Jesus loved, and we witness a macabre combination ordination and adoption ceremony: Woman, behold your son. Son, behold your mother.
Strange and unsettling things can happen at the foot of the cross.
This was not, of course, either the first or last execution designed as spectacle. Until recent times, executions almost always drew a crowd. That was part of the point. For a long time, executions were specifically designed for maximum public effect. Sometimes, like Jesus' execution, these public spectacles were organized for easy public access to discourage similar insurrectional impulses, or to placate the public's perceived need for retributive justice, or to terrorize people into submission to authority.
But truth be told, executions also provided huge sources of public entertainment. I suspect that was the case for at least some of the bystanders and the curious who gathered on Golgotha. There were public executions at the hanging ground at Tyburn in London right through the 18th century. There were well-attended beheadings by guillotine during the Reign of Terror in Paris in what is now ironically named the Place de la Concord. Those were the better-known spectacles.
We in this country, of course, have our own bloody stories to tell. There were those dreadful, hateful lynchings of black citizens in the American South. Those events, too, were treated by spectators as entertaining sideshows. You can see that for yourself in the surviving photographs that circulated for months after each event, sent through the mail as sordid postcard souvenirs. Repressed desire and vile racist hatreds are everywhere in evidence on the faces of witnesses in those photographs, lazily munching their boiled peanuts as they hoist their children to their shoulders for a better view of the swinging corpse.
It's always been a bit crowded at the foot of the cross.
Until recently, that is. One of the ironies of the current legal practice of capital punishment is that it has gone strangely private. If Jesus were on death row today, Mary and the beloved disciple could not get close to him even if they tried. Witnesses to these spectacles are few, and getting fewer. I don't know whether you have been following the stories out of Arkansas. It seems that starting on Monday, Arkansas intended to execute eight convicted criminals, two a day, by chemical injection. They are in a hurry because the supply of midazolam, one of the three lethal chemicals used in such executions, expires on April 30, and drug makers have pretty much cut off any further supply. The Arkansas Department of Corrections is eager to use what's in stock before the well runs dry. But according to an NBC report that came out a few weeks ago, there's a catch. The law requires that at least "six respectable citizens" must view the executions to confirm that they "are conducted in the manner required by law." But they were having trouble finding the 48 witnesses they needed. The director of the department even paid a visit to the regular meeting of the Little Rock Rotary Club to find volunteers. The Rotary Club president told NBC that at first there was a little laugh from the audience, because they thought she was kidding. It quickly became obvious that she wasn't. The Department now says that people could double up, which would reduce the numbers of witnesses required. I take it as a good sign that no Rotarian came forward, which means the whole thing might end up delayed.
O Savior of the world,
We, too, gather here as witnesses, but not the kind of witnesses that the authorities in Little Rock are trying so desperately to gather. We gather here as witnesses willing to testify to the richness of God's mercy, to the depth of God's compassion—a compassion revealed in the broken body of the crucified one, a broken body that gives hope to all the broken bodies of this world: to those who suffer, to the oppressed, to the hungry and thirsty, to the exiled and the refugee, to all who live in fear in this city, to all those for whom our prayers have been requested, for all those intentions that we will now lay at the foot of the cross.
If you wander through the galleries at the Art Institute, it won't take you long to find paintings of the Crucifixion. Most of them devote a lot of canvas to depicting the crowd. The image on today's service leaflet was painted 500 years ago in Germany by Lucas Cranach, a close friend of Martin Luther's. You might notice that Cranach has divided the crowd pretty decisively, as if he were painting a scene of the Last Judgment. He puts the good people (and the good thief) at Jesus' right hand, all of them focused on the cross. On Jesus' left, there's a pretty sinister crew, looking pretty much every way but up. That kind of black and white thinking is all too familiar to us these days, a judgmental polarizing for which our country—like Cranach's Europe 500 years ago—seems poised to reap the whirlwind. It's probably the least attractive aspect of this image.
But then you notice the two people Cranach positions directly below Jesus feet. You see a father standing with his young son, the father's hand pointing upward. They stand on neither one side nor the other. The father wants to be sure that the boy isn't distracted by the noise and dust and tears that surround him. He wants his son instead to keep his eye on what matters most, on the dying criminal who is no criminal, the suffering God who now, lifted up, for better or for worse, draws all humanity to himself. As the father directs the young boy's gaze, so Cranach directs ours.
Which brings us back to this time, to this room, and to the ritual action that will soon take place. You will notice in Cranach's picture that the people gathered at the foot of the cross are not wearing first-century costumes. Neither are we. We gather here in our ordinary clothes, as our ordinary selves—or as the hymn declares, we gather just as we are. We gather first to lay our petitions at the foot of the cross, those simple sealed envelopes that contain the mute but eloquent testimony of our failings and our desires, of our penitence and our gratitude. In so doing may we also present ourselves, our souls and bodies, as agents of justice and reconciliation, trusting in God's mercy and loving kindness even here, at the foot of the cross, even in these dark and perilously divided days.
Save us and help us, we humbly beseech thee, O Lord


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Orange is the New Black 1.02: Tit Punch
Continued from Page 2 of Orange is the New Black 1.02: Tit Punch
Flashing back to happier times for Piper, she and her friend Polly are where all women should be: in the kitchen with aprons. Ha ha ha...oh wait, no, that's terrible. Regardless, they both are apron-ed out and apparently making homemade soap. Is this what upper middle class white women do for fun?
Polly's delightful husband Pete is also present, and when Piper mentions Larry, Pete asks, "You still with that guy? Thought you wouldn't make it two months." Oh Pete, I like you. When Polly admonishes him, Pete says, "What? You said so too." Oh Pete, I
really like you. Polly announces, "They're moving in together," clearly trying to urge Pete to shut his trap from hereon out. Doing the opposite, Pete asks, "Already? Shit. You are still a lesbian." That's it. Within seconds, Pete is officially my favorite. Well done, sir.
In reaction, Piper gives Pete a sly smile and she receives an adorable peck on her cheek from Pete before he goes off running. Gah, I love him. Once he's gone, Piper looks around at Polly's handywork and the proverbial light bulb appears above her head. She tells Polly, "You could sell these, you know? At farmer's markets...little boutique stores. I could be your partner. This could be something. I mean, this could be a thing, Pol. Market it right, and package it right; this is money." You little entrepreneur, you. Polly adorably adds in a whisper, "I make lotions too." Man, I want to be besties with Pete and Polly. They're both individually and jointly wonderful. These are some straight marrieds I can get behind.
Back to the present day nightmare Piper is living in, she is lined up
Piper: I am as high as a kite
waiting for commissary, hoping to be able to purchase something. Nichols comes up from behind to inform Piper that the "Spanish ladies" are now referring to her as "the wailing lady." Nichols, that's not helping. Piper responds, "Well, they would have screamed just as loud if someone handed them a used tampon sandwich." Agreed.
Nichols: "Or if they suddenly saw an ex-girlfriend in prison. What's her name? Alex?" At this, Piper's head snaps back around so quickly, it almost comes off. Piper demands, "What did she say to you?"
Nichols: "Not a word. I just know dyke drama when I see it." This is accompanied with another slick wink of the eye. Do they have winking classes in prison? Where is this coming from? Also, true enough. If anyone knows dyke drama, it'd be born-to-play-gay Natasha Lyonne. When Piper finally makes it up to the commissary window, her money still hasn't processed, but Nichols does her a favor and lets her get some non-food items. Aw, that was nice of you, Nichols.
Next we see LCF's best hairdresser Sophia working on Taystee's post-brawl hair. Taystee complains, "I paid you seven bottles of Pantene for this shit." Taking zero of Taystee's shiz, Sophia lays down the truth, "Ain't my fault you went all UFC over a King Cone. And if you call it 'shit' one more time, you can take your ass down to Denita." Game, set, and match to Sophia.
Hey ladiesssss...
Why is she still here?
Then, in walks a very smiley Piper who awkwardly opens with, "Hi, I'm Chapman." This is met with looks that make it known that Piper's reputation precedes her. And that ain't a good thing. Piper asks Sophia if she has cocoa butter or shea butter available for trade. Sophia is wearily open to the idea and tells her what the cost of her request is - all items from commissary. Piper happily informs Sophia, "Gladly, I will get them to you the second that my money comes in." This results in a loud cackle of laughter from Taystee and a "Credit declined" from Sophia. The store is now closed.
Piper begs, "Please," which only leads to Sophia commenting, "'Please' is for commissary hos and Oliver Twist." Snort. I think that means "no," Piper. Fortunately for her though, Taystee finds a solution to both her and Piper's problem. What is this solution? Some of her golden yellow hair in exchange for some of her commissary. Taystee's happy; Sophia's paid; and Piper's creepily content as well. All in all, the barter system is alive and well in LCF!
Once she has accumulated some of her supplies, Piper returns to her room, checking out her underwear to see if it'll suffice as a filter. From behind appears Suzanne "Crazy Eyes" Warren. Crazy Eyes asks "Are you the new girl?" Flipping right around, Piper
You wouldn't happen to be interested in some "real talk," would you?
hesitantly answers, "Yes, I am. Piper." Crazy Eyes continues to stand there looking as if she has sustained a concussion, with her eyes bizarrely unable to focus. Piper goes on to ask, "And you are?"
"Uh, Sue. It's short for Susie, which is short for Suzanne," rambles Crazy Eyes, while making a myriad of nonsensical hand motions. She asks Piper, "You like spicy food?"
Piper, with fear in her voice, replies, "Sometimes."
Crazy Eyes: "One of my girlfriends, she was Mexican. Real talk." Oh, how nice. I've been waiting for some "real talk."
Crazy Eyes: "Uh, she gone now, but she left these." In her hand are three peppers - exactly what Piper has been looking for. Random question - how long has this Mexican girlfriend been gone? Because those peppers appear to be ripe, so it cannot have been that long. Just askin'.
When Piper tells her she has nothing to exchange for the peppers, Crazy Eyes sweetly says, "People forget we was all new here once.
It's good to know you ain't alone," and hands them over to Piper. And with that, Crazy Eyes' "Phase 1" of seduction is complete. Nicely done.
A flashback then takes us back to the middle of detox week for Piper and Larry. Larry appears to be loving the detox and Piper looks like she wants to crawl in a hole and die. I would be like Piper. Well, if I did a detox, which I would never do. Piper not-so-subtly asks, "What if we only did this for five days?" Larry, with accusation in his voice, asks, "You wanna cut it short?"
"Not cut it short. Just...yes," admits Piper with an unsettling grin on her face. Ah, so that's how you smile through defeat.
The moment right before Piper murders Larry
Piper "Needs to Get off Detox" Chapman
When Larry goes to give Piper a kiss on the cheek, a familiar scent wafts into his nostrils. Leaning back in for another sniff, Piper tries to deflect, "You are not a werewolf." Oh Piper, tell me that's not your sad way of trying to get him to halt his investigation. After his second confirmation smell, Larry pulls back and looks at Piper directly in the eyes, stating, "Fucker." Piper confesses to
cheating on the detox with Mr. Fox's Honey Barbecue Pork Rinds. Wow, when that girl cheats, she doesn't half-ass it; she goes all the way (*cough cough red flag for you Larry *cough cough). Disgusted with her, but eventually turned on by her porcine aroma (as all carnivores are), the two of them share in a weird pork rind breathe-a-thon before lightheartedly getting their affection on. I'll admit it...they're kinda cute, and they seem like they legitimately are in love. Damn you straight white couples! (*shakes indignant gay fist) Somehow tricking me into supporting you...I'm so weak.
Cut to the present, where Piper is not-so-silently sobbing alone on her top bunk bed. Pornstache just so happens to be passing by the room, and being Mr. Wonderful, he takes time to mock Piper: "Awwww, don't be so sad. Poor little bay-bay." Piper glares back at him contemptuously, but her stone cold demeanor loses some "cool" points as a strand of her hair is still sticking to the snot bubbles on her face. I hate when that happens.
So...things are going great!
We then see that she's actually chewing on one of the peppers from Crazy Eyes and then regurgitating it into her underwear filter. Um...what? I hope this leads somewhere good because right now, everything just seems horrific. Piper seems to agree as she continues to sob and chew and sob and chew. It's what dreams are made of.
Continue to Page 4 of Orange is the New Black 1.02: Tit Punch


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Tennis Garden Cures Monday Blues
Posted by Cindy Uken | Mar 11, 2019 | Valley Life
INDIAN WELLS — All eyes will again be on the Indian Wells Tennis Garden this week as world-class tennis takes center stage in the Coachella Valley and around the world.
If you have a case of the Monday blahs, head to the Indian Wells Tennis Garden. Stadium 1 has a lineup sure to lift your spirits. Monday, March 11 appearances include World No. 1 and defending champion Naomi Osaka who takes on Danielle Collins, an all-American matchup between Venus Williams and Christina McHale and World No. 1 Novak Djokovic will do battle with Philipp Kohlschreiber.
Waste no time. Get your tickets by clicking here.
Venus Williams will continue her run in the desert on Monday afternoon against fellow American Christina McHale. Fresh off of her stunning second round upset of World No. 3 Petra Kvitova on Saturday night at the Indian Wells Tennis Garden, Williams will return to Stadium 1 as the center of attention.
When the two Americans meet, it'll be the first match they've ever played across the net from one another, according to the BNP Paribas. While each is vying for the same goal at the Indian Wells Tennis Garden, that's about all Williams and McHale have in common.
With match-ups, competition and big names like this, it's little wonder the tennis garden and its event is grabbing national and international headlines.
A headline on Forbes.com exclaimed, "Indian Wells Growing A Singular Tennis Experience."
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text:
\section{Introduction}

The SKA Simulated Skies project ($S^3$) aims at building mock radio skies suitable for planning science with the SKA and the many pathfinder experiments. The project comprises a number of simulations, of which essentially two are relevant for this paper:

$\bullet$ $S^3$-SEX ({\bf S}emi-{\bf E}mpirical e{\bf X}tragalactic) : a large-scale simulation of the extragalactic radio continuum sky covering a sky area of $20^{\circ} \times 20^{\circ}$, out to redshift $z=20$, and down to 10 nJy. It also includes {\sc Hi} gas masses for star-forming galaxies. For a complete description, see \cite{wilman08}.

$\bullet$ $S^3$-SAX ({\bf S}emi-{\bf A}nalytical e{\bf X}tragalactic) : a smaller-scale simulation of the extragalactic {\sc Hi} and CO line emissions, derived from the Millenium simulation (\cite{springel05}), which comes in two flavours. $S^3$-SAX-Sky is a skyfield simulation giving the apparent properties of galaxies, with a field of view that depends on the maximum redshift, while $S^3$-SAX-Box is a simulation of a cubic volume giving their intrinsic properties. In all of this paper, $S^3$-SAX shall be understood as meaning $S^3$-SAX-Sky. For a complete description, see \cite{obreschkow09}.

\section{Querying the $S^3$ databases}

\subsection{Database structure}
The databases can be queried via SQL forms on the dedicated $S^3$-SEX and $S^3$-SAX sections of the $S^3$ website hosted at {\tt http://s-cubed.physics.ox.ac.uk}. The queries should be written in the SQL format, and query examples are given.

The $S^3$-SEX and $S^3$-SAX databases have similar structures, and consist of respectively three and two tables.

$\bullet$ For $S^3$-SEX : a {\sf Clusters} table holding cluster properties, a {\sf Galaxies} table holding galaxy properties (possibly including the cluster index to which they belong) and a {\sl Components} table, which lists the properties of the several components that may make up a single galaxy, such as cores and radio lobes.

$\bullet$ For $S^3$-SAX : a {\sf galaxies\_line} table containing the apparent position and emission line properties of the galaxies and a {\sf galaxies\_delu} table containing the intrinsic properties of the \cite{delucia06} catalog.

For more information on the structure of the database and the attributes held in the various tables, please refer to the appropriate sections of the $S^3$ website. It is advisable to do so before reading on, as in the following we shall mention some of these attributes explicitly.

\subsection{Mandatory attributes}
\label{sec:mandatoryitems}
To make maps from these simulations, it is mandatory that some properties - listed below - be included in the query, as the mapping algorithms require them :

$\bullet$ For $S^3$-SEX :

\noindent
In the {\sf Galaxies} table : {\sf galaxy}, {\sf redshift} or {\sf modified\_redshift}, {\sf distance}, {\sf sftype}, {\sf agntype} (these latter two are necessary if one wishes to make separate images for the different types of sources), {\sf m\_hi} (if {\sc Hi} mapping is to be performed).
\\
In the {\sf Components} table : {\sf galaxy}, {\sf right\_ascension}, {\sf declination}, {\sf position\_angle}, {\sf major\_axis}, {\sf minor\_axis}, {\sf i\_151}, {\sf i\_610}, {\sf i\_1400}, {\sf i\_4860}, {\sf i\_14000}.

$\bullet$ For $S^3$-SAX :

\noindent
In the {\sf Galaxies} table only : {\sf ra}, {\sf decl}, {\sf zapparent}, {\sf diskpositionangle}, {\sf diskinclination}, {\sf rmolc}, {\sf distance}. To these, one should add {\sf hiintflux}, {\sf himajoraxis\_10max}, {\sf hiwidth50} and {\sf hiwidth20} for mapping the {\sc Hi} line, as well as {\sf cointflux\_$J$}, {\sf h2majoraxis\_10max}, {\sf cowidth50} and {\sf cowidth20} for mapping the CO($J\to J-1$) line. When using the Kapteyn {\sc Hi} templates (see below), {\sf hubbletype} should also be retrieved.

\subsection{Structure of query result files}

Query results are saved in a gzipped tarball {\tt id.tar.gz}, where {\tt id} is a hash given by the server at submission time. The tarball contains two plain text files : {\tt id.sql}, in which the original SQL-formatted query is recalled, and {\tt id.result}, which contains the comma-separated query results proper.

\section{Installing the $S^3$-Tools}

\subsection{Prerequisites and installation}
The $S^3$-Tools are currently hosted on an external website at {\tt http://www.lra.ens.fr/$\sim$levrier/Recherche/S3/}, although they should find a permanent home on the $S^3$ webserver in the near future.

To install the $S^3$-Tools, you should refer to that website or to the README file included in the distribution. In particular, the user should be aware that the $S^3$-Tools require a number of python libraries, namely the scipy, numpy, os, math and pyfits packages. For Mac users, these are all included in the SciSoft package (at least from version 2008.3.1 onwards) for OS X.

Provided these packages are functioning properly on your system, installation is a simple matter of untarring the {\tt S3Tools.tgz} archive and setting a few paths in the {\tt Config\_Path.py} file in the {\tt Config/} subdirectory. In the following, we shall assume that installation is done in a directory named {\tt S3Tools} under your home directory. Configuration files should therefore be in {\tt $\sim$/S3Tools/Config/} and the main routines in {\tt $\sim$/S3Tools/Routines/}.

\subsection{Templates}
\label{sec:templates}
To make line maps from $S^3$-SAX, {\sc Hi} and CO templates are required. These were made by D. Obreschkow and are available on the same webpage. Be warned that the archive weighs over 2~GB. A different set of templates for {\sc Hi} has been produced by R. Boomsma from Kapteyn Institute and are also readily available to use.

\subsection{Global Sky Model}
\label{sec:gsm}

The Global Sky Model (GSM) - also dubbed $S^3$-GAL on the $S^3$ website - is a model of the Galactic foregrounds from 10 MHz to 100 GHz by \cite{deoliveiracosta08}. It is possible to include these foregrounds in spectral cubes built from the SKA Simulated Skies with $S^3$-Map. To be able to use this option, the GSM data and routines should be installed from the GSM website {\tt http://space.mit.edu/home/angelica/gsm/}, and the installation directory specified via the {\tt GSM\_DIR} variable in {\tt Config\_Path.py}.

\section{Making maps and spectral data cubes}

\subsection{The $S^3$-Map GUI and underlying scripts}

Making maps from query results is done via $S^3$-Map, a graphical user interface (GUI) written in python, which is run by moving to the {\tt Routines/} subdirectory and typing {\tt python S3Map.py} at the command line. A window similar to the one presented in Fig.~\ref{fig:S3Map} should appear after a few moments. It is through this interface that users specify which maps to make. To be more specific, the state of the GUI is passed as arguments to a python script command, either {\tt SEX\_map\_script.py} or {\tt SAX\_map\_script.py}. It is this command that is in charge of actually building the maps using lower-level routines, and it may be printed out on the screen by clicking on the {\sf Show} button. The user can then copy-paste this command into a terminal window and perform the same mapping non-interactively. This is a useful trick to know for building batch jobs or debugging purposes. For a lengthy description of the syntax used for the arguments, please refer to the $S^3$-Tools user's guide.

\begin{figure}
\centering
\includegraphics[width=7cm]{S3Map2.eps}
\caption{The $S^3$-Map graphical user interface}
\label{fig:S3Map}
\end{figure}

\subsection{Common workings of the $S^3$-Map GUI}

Click on the {\sf Browse} button to select a tarball containing results from a database query. This prompts $S^3$-Map to check which database was queried, so that some of the buttons, menus, entries and options become either active or inactive, depending on their relevance. $S^3$-Map also fills in the mapping area fields with extremal values for right ascension ({\sf X}), declination ({\sf Y}) and redshift ({\sf z}) found in the query results. The {\sf From Query} checkboxes are then set, but the user may deactivate them and manually specify  a different mapping area.

Regarding frequency configuration, this is done via three entry fields : {\sf Minimum Frequency} (central frequency of the first channel), {\sf Frequency Resolution} (full channel width) and the number of channels. For line mapping, a convenient\footnote{"That {\sf Setup} button is a stroke of genius" (I. Heywood {\it dixit}).} {\sf Setup} button has been included : Simply select which line in which redshift range to look for and the number of channels to use, {\sf Setup} automatically adjusts {\sf Minimum Frequency} and {\sf Frequency Resolution} for you.

The user also has the possibility of putting in the effects of a Gaussian beam, via the {\sf Beam Major FWHM}, {\sf Beam Minor FWHM} and {\sf Beam Position Angle} entry fields. Please note that a beam smaller than the pixel size specified in the corresponding field has of course no effect. In that case, no convolution is performed.

Gaussian noise can be added to each frequency plane in the output spectral cube. This is done via the dedicated {\sf Noise level} entry field. Currently, the said noise level sets the ratio of the added noise's rms value to the maximal value of the noiseless map.

It is also possible to add the Galactic foreground signal at each frequency form the Global Sky Model described in \ref{sec:gsm}. For this, simply tick the {\sf Global Sky Model} checkbox. Be aware that this is much lower spatial resolution than the SKA Simulated Skies, and so may appear in most cases as just an added constant over the requested skyfield.

The unit of the third axis can be set, using the {\sf Z-axis} menu, to one of frequency, velocity or wavelength. The user should be aware that the "velocity" option only applies to the mapping of a single line. If this option is selected while requesting the mapping of several lines or no line, the script will revert to a frequency axis.

The usual convention for the orientation of the right ascension axis is that it increases to the left (i.e. to the east). This can be changed by ticking the {\sf Reverse R.A.} checkbox.

Finally, to use the mapped field as input to instrument simulators, the user has a possibility to specify the pointing corresponding to the center of the map. This is done using the {\sf Map Center} entry fields at the bottom of the GUI. When the checkbox next to it is off, this pointing is not used and the positions found in the query result are used. Considering that the simulations are centered on (0,0), this may lead to strange behaviour in later stages of the end-to-end simulations, and it is therefore not recommended.

\subsection{Some points specific to $S^3$-SEX}

\subsubsection{Elliptical templates}

In $S^3$-SEX, sources are made up of components that are either ellipses or point sources, and each line in the query results file corresponds to such a component. As mentioned in \ref{sec:mandatoryitems}, the information given for each component includes position, major and minor axes, position angle, continuum fluxes at the reference frequencies, and possibly {\sc Hi} mass. Given a window and a pixel size for the desired map, we can build a template image for each single component by setting to one the values of pixels whose centers fall within the ellipse, and to zero all other pixel values.

This approach is fine if the component's size is much smaller or much larger than a pixel. In the former case only one pixel is non-zero, and in the latter case, the component's border in the template image resembles the desired ellipse quite closely. A problem arises with components whose sizes are a few pixels across, as can be seen on the left side of Fig.~\ref{fig:accuracy}.

\begin{figure}
\centering
\includegraphics[width=8cm]{accuracy.eps}
\caption{Dealing with image accuracy for few-pixel components. {\it Left :} without regridding ; {\it Right :} with regridding.}
\label{fig:accuracy}
\end{figure}

To correct for this, the grid is temporarily refined, as on the right side of Fig.~\ref{fig:accuracy}, with a minimum ratio of semi-major axis to refined pixel size given by the value of the {\sf Image accuracy} entry field on the GUI. Then each coarse pixel in the original grid is given a value proportional to the total number of non-zero refined pixels that belong to this coarse pixel.

In all cases, the template image is then normalized so that the integrated flux over the component is 1 Jy, and convolved by a flux-conserving beam.

\subsubsection{Continuum and {\sc Hi} fluxes}

Simultaneously, the continuum flux at the desired frequency - or frequencies - is computed from a log-polynomial interpolation based on the reference fluxes retrieved from the query results.
As for the total {\sc Hi} flux, it has to be derived from the {\sc Hi} gas mass and distance using
$$
\int \frac{S\mathrm{d}v}{1~\mathrm{Jy.km.s}^{-1}}=4.24\times 10^{-6} \left(\frac{M_{HI}}{M_\odot}\right)\left(\frac{D}{\mathrm{Mpc}}\right)^{-2},
$$
and a synthetic double-peaked profile, is built randomly using some prescriptions based on galaxy type\footnote{For more detail, please refer to the user's guide.}. The {\sc Hi} flux in each frequency channel is computed by integration of this synthetic profile over the channel's width. The total (continuum+{\sc Hi}) flux is then used to multiply the template image at each of the desired frequencies, to obtain a spectral data cube which is finally pasted onto the overall cube.
This means that the emission profile is painted uniformly over the galaxy's disc. This approach is sufficient at low spatial resolution.

\subsubsection{Polarized continuum emission}

By default, only total intensity continuum emission is mapped, but in the {\sf I,Q,U,V} menu, the user may specify that linearly polarized emission should be mapped as well. This emission is computed from the source's total intensity and observing frequencies by routines included in the $S^3$-Tools and which were kindly provided by J\"orn Geisb\"usch (Cavendish Laboratory, Cambridge University). In that case, the output cube has a fourth dimension, with separate Stokes I, Q and U hyperplanes. In the algorithm, for each source, the same template built for total intensity is used for Stokes Q and U, it is simply multiplied by the appropriate fluxes.

\subsubsection{Source types}

There are 5 different source types in the $S^3$-SEX simulation (Radio-quiet AGN, FRI and FRII radio-loud sources, quiescent star-forming galaxies and starbursting galaxies) which are distinguished via their {\sf sftype} and {\sf agntype} attributes. The user can choose to map only selected types by using the {\sf Source Types} pull-down menu. Obviously, only those source types which were queried can be mapped, and the {\sf sftype} and {\sf agntype} must have been included in the query for the selective mapping to be possible. On a related note, GPS sources are a subclass of the FRI and FRII source types (see \cite{wilman08}). The user may specify whether these should be included or excluded, using the {\sf GPS} menu.

\subsection{Some points specific to $S^3$-SAX}

The {\sc Hi} and CO emission maps from $S^3$-SAX data require, as mentioned in \ref{sec:templates}, a number of position-position-velocity (PPV) templates. For {\sc Hi}, the user has the choice between templates from D. Obreschkow ({\sf Oxford} option in the {\sf HI Data} menu) or templates from R. Boomsma ({\sf Kapteyn} option). For CO, only templates by D. Obreschkow are available. They are included in the archive along with the {\sc Hi} templates.

Ten $J\to J-1$ rotational transitions of CO ($J$ going from 1 to 10) are available in the database and can be queried. The queried lines are active in the {\sf Transitions} menu, and by default they are selected for mapping.

In all cases, for a given galaxy, the relevant template is retrieved based on the values of {\sf hubbletype}, {\sf rmolc}, {\sf himajoraxis\_10max}, {\sf h2majoraxis\_10max}, {\sf diskinclination}, {\sf cowidth50} and {\sf hiwidth50}, then submitted to necessary up- or down-scaling in the spatial and velocity dimensions, rotation and normalization to the integrated line flux. The template is eventually pasted onto the output cube.

\section{Upcoming extensions}

The remaining items on the agenda for the $S^3$-Tools are :

$\bullet$ Inclusion of the epoch of reionization (EoR) signals produced independently by M. Santos (IST Lisbon) and B. Semelin (Observatoire de Paris / LERMA). This will be very similar to the way the GSM is included.

$\bullet$ Inclusion of polarized emission in $S^3$-SAX via templates produced by R. Beck and T. Arshakian (MPIfR)

$\bullet$ The mapping scripts currently deal with one source at a time, building or finding a template, transforming it and pasting it onto the master cube. Obviously, this could be parallelized.

$\bullet$  An older version of the $S^3$-Tools included annotation files for the KARMA visualisation software. This should eventually be re-included.

$\bullet$  The mapping scripts should be installed on the $S^3$ web server and a front-end form similar to the GUI developed for the website. This would allow users to request maps from the server without having to download and install the $S^3$-Tools.

$\bullet$  A better treatment of {\sc Hi} in $S^3$-SEX is possible, for instance by using {\sc Hi} surveys such as HIPASS to derive synthetic line profiles consistent with observations.

\begin{acknowledgements}
This work was supported by the
   European Commission Framework Program 6, Project SKADS, Square
   Kilometre Array Design Studies (SKADS), contract no 011938.
\end{acknowledgements}

redpajama_set_name: RedPajamaArXiv


text:
Measured wideband characteristics of indoor channels at centimetric and millimetric bands
Wei Fan1,
Ines Carton1,
Jesper Ø. Nielsen1,
Kim Olesen1 &
Gert F. Pedersen1
Accurate characterization of spatial multipath channels at millimeter wave bands has gained significant interest both in industry and academia. A channel measurement was conducted at three different frequency bands, i.e., 2−4, 14−16, and 28−30 GHz in a line-of-sight (LOS) and an obstructed-LOS (O-LOS) scenarios in an empty room environment. A vector network analyzer connected to a virtual uniform circular array and to a rotational directional horn antenna was used in the measurements, respectively. Angle-of-arrivals and delay-of-arrivals of the multipath components were obtained from the measurements for the three frequency bands. Room electromagnetic properties for the three different frequencies at different propagation scenarios were investigated as well.
The increasing demand for higher data rates has motivated research in millimeter wave frequency bands for 5G cellular systems. Millimeter wave bands offer huge free spectrum and allow the implementation of massive antenna arrays due to the small wavelength [1, 2]. Though broadband wireless access technology local multipoint distribution service (LMDS) already exists at 28 GHz, it is still unused. This band has been considered as a potential candidate for 5G cellular frequency due to its low atmospheric absorption, and availability of high gain adaptive antennas [3–6]. Accurate characterization of their spatial multipath channel at millimeter wave bands has gained significant interest both in industry and academia, as it is important for system design and performance analysis of future millimeter wave communication systems [7, 8].
While significant studies of channel characteristics were carried out at 60 GHz for indoor and short-range scenarios, only a few measurement campaigns were conducted at 28 GHz [9, 10]. Various measurement results have been reported for the 28 GHz band in the literature for urban scenarios, e.g., 28 GHz penetration and reflection measurement in [1, 3], 28 GHz path loss and signal outage analysis in [1, 11], 28 GHz angle of arrival and angle of departure analysis in [1, 5], etc. Measurement results in an indoor building-scale environment based on a home-made synchronous channel sounder were reported in [6]. To the best knowledge of the authors, very few papers have experimentally investigated the channel characteristics at 30 GHz. Measured results of indoor propagation channels at 30 GHz were reported in [12, 13], where the focus was only on path loss and small-scale fading characteristics.
Extensive work has been done for channel characterization in the literature at current cellular frequencies [14, 15] and other frequency bands, e.g., 5.8 GHz in [16, 17]. The existing work in the literature, however, are lacking in the analysis on the frequency-dependent channel behaviors. The frequency dependency factor is important, as the larger bandwidth, e.g., several GHz or subbands separated by GHz, might be utilized for future wireless systems. It would be highly interesting to compare the channel characteristics at current cellular frequency bands and at millimeter wave bands in the same propagation scenarios.
Room electromagnetics is a simple model that considers a line-of-sight (LOS) component (if present) and an exponential power-delay profile (PDP) decaying with the so-called reverberation time parameter, depending only on the wall area, the volume of the room, and an absorption coefficient. Room electromagnetics theory is interesting, as it does not require complete knowledge of the propagation environment, and it offers an alternative description of diffuse scattering in a room using only simple parameters. Validation of room electromagnetic theory was investigated for cellular frequencies [18–20]. However, very few results are available in the analysis on frequency dependency of room electromagnetics.
In this paper, we investigate the spatial-temporal characteristics of LOS and obstructed-LOS (O-LOS) scenarios in an indoor environment at three different frequency bands, namely, 2−4, 14−16, and 28−30 GHz. Angle-of-arrival and delay-of-arrival of the main paths and room electromagnetics are investigated for different frequency bands. Through the extensive measurements, we would like to investigate: (1) whether channel characteristics at different frequency bands are different in the same propagation scenario; (2) whether room electromagnetics theory holds at different frequency bands; and (3) whether diffuse scattering is important to model at millimeter wave frequency bands.
The main contributions of the paper are summarized as follows:
A sounding system using a VNA coupled to a virtual uniform circular array (UCA) and to a rotational directional antenna to resolve multipath components in delay and spatial domains at different frequencies is described.
Spatial-temporal characteristics of the indoor channels at different frequencies are compared in LOS and obstructed-LOS scenarios. The trajectory of multipath components in a room are identified by relating the multipath angle and delay information to the room geometry.
Room electromagnetic parameters at different frequencies are compared in LOS and O-LOS scenarios.
Spatial multipath components estimated with a virtual UCA are compared with results obtained with rotational directional antenna measurements.
Virtual arrays (via mechanical displacement of a single Biconical antenna) and rotation of this paper is organized as follows. Section 2 describes the indoorpropagation channels and the frequency beamforming technique used to estimate the spatial and temporal properties of multipath channels. Section 3 discusses the measurement setup. Section 4 summarizes the measurement results. Finally, section 5 concludes the paper.
Indoor propagation channels
To resolve the multipath components in space, two measurement systems are generally used. One is to steer a highly directional antenna to scan the channel impulse response (CIR) from each angular direction. This gives the angle information of the channel directly. However, the disadvantage is that the antenna pattern is embedded into the results. The other method is to use an (virtual) array. The angle information of the multipath components can be obtained via beamforming or high-resolution algorithms [21]. A uniform circular array (UCA) is preferable to a uniform linear array (ULA), as the ULA cannot distinguish the paths symmetric with respect to the array line and the beam pattern of the ULA array is not uniform around the azimuth angle.
For static indoor measurements, the measured CIR is essentially only one snapshot of an environment, i.e., only one temporal observation is available. The spatial method discussed in [22], e.g., the classical beamforming and high resolution algorithms like MUSIC cannot be directly applied, since the covariance matrix of the array outputs would be rank-deficient due to the limited temporal samples. Different algorithms were proposed to address this issue, e.g., a spatial smoothing technique in [21] and an iterative 2D Unitary ESPRIT method in [23] for virtual planar arrays. In this paper, we are interested in both delay and angle information of the multipath components. For the sake of simplicity, a conventional frequency beamforming algorithm is used [24]. Note that frequency beamforming algorithms were only used to estimate the angle and delay of the direct path between the transmitter (Tx) and receiver (Rx) for indoor ranging and localization purpose in [24].
Assume a UCA with P array elements arranged uniformly around its perimeter of radius r, each with angle θ i =2π·i/P with i∈[0,P−1] as illustrated in Fig. 1. Note that the distance between two consecutive array elements should not be larger than λ/2 to avoid spatial aliasing effects [22]. Assume that the CIR between the Tx and the center of the UCA is composed by K multipath plane waves. The channel frequency response is:
$$ H(f)=\sum\limits_{k=0}^{K-1}\alpha_{k}\exp\left(-j2\pi f\tau_{k}\right), $$
An illustration of the UCA and the multipath channel
where α k and τ k represent the complex amplitude and delay of the kth wave with k∈[0,K−1]. The k-th wave impinging with angle of arrival φ k arrives at the i-th element with a delay \(\tau _{k_{i}}\) with respect to the UCA center:
$$ \tau_{k_{i}}=-\frac{r\cdot\cos\left(\theta_{i}-\varphi_{k}\right)}{c}, $$
where c is the speed of light. The frequency response H i (f) at the ith element can be written as:
$$ H_{i}(f)=\sum\limits_{k=0}^{K-1}\alpha_{k}\cdot\exp\left[-j2\pi f(\tau_{k}+\tau_{k_{i}})\right] $$
The array frequency response H(f,θ) is:
$$ H(f,\theta)=\frac{1}{P}\sum\limits_{i=0}^{P-1} w_{i} H_{i}(f), $$
where w i ,i∈[0,P−1] is the complex weight assigned to the ith antenna element. The basic principle of classical beamforming is to shift the phase of each frequency response into alignment. Therefore, the weighting vector can be expressed as:
$$ w_{i} = exp\left(-j 2 \pi \cdot (r/c) \cdot cos(\theta - \theta_{i})\right), $$
A power peak occurs in the array beam pattern for θ=φ k . The spatial-temporal channel impulse response h(t,θ) can be recovered from H(f,θ) via inverse discrete Fourier transform:
$$ h(t,\theta)=\sum\limits_{n=0}^{N-1}H\left(f_{n},\theta\right)\cdot\exp\left(j2\pi f_{n}t\right), $$
where f n is the frequency at the n-th frequency index.
Experimental setup
Figure 2 illustrates the block diagram of the measurement system. A wideband biconical antenna was mounted on a table as the transmitter (Tx), while two types of antennas were used as the receiver (Rx). Note that both the Tx and Rx antenna were mounted at a height of 1.1 m above the ground. With the two different Rx antennas, two sets of measurements were performed. In the first measurements, a uniform circular array (UCA) was realized virtually by mounting a biconical antenna on a positioning turntable. We obtained P=720 elements of the UCA array by automatically repositioning the biconical antenna at uniform angles around a circle perimeter with r=0.5 m. At each element position, a frequency sweep was performed for three different frequency bands 2−4, 14−16, and 28−30 GHz. N=750 samples were set for each frequency band. In the second measurement series, a horn antenna was mounted on the rotation center of the turntable. To make meaningful comparison, the same measurement settings as in the first measurement series (i.e., the same frequency sweep and orientation sweep) were adopted for the second measurement series. A complete channel measurement, i.e., frequency sweep over the three bands for all element positions, took about 15 min. Three types of antennas were used in the measurement campaign, as detailed in Table 1. The biconical antenna is omnidirectional in the azimuth plane for 2−30 GHz, while the beamwidth gets narrower in the elevation plane as the operating frequency increases. The horn antenna operating at 750 MHz – 18 GHz frequency band is less directional at the low band both in azimuth and elevation plane, and becomes more directional as the frequency increases. The horn antenna operating at 26.4−40 GHz has approximately the same beamwidth in the elevation and azimuth plane. All the antennas used in the measurements are vertically polarized.
Block diagram of the measurement system. The measurement system consists of a VNA, a LO/IF distribution unit, two reference mixer modular. The mixer modular is used to down-convert the received signals at the Rx to a lower frequency to reduce the cable loss and phase variation at the long cable (9 m). Calibration was performed prior to measurements to de-embed the Tx and Rx chain in the measurement results. Channel frequency responses at three frequency bands were recorded over one sweep
Table 1 Specifications of the antennas used in the measurement campaign
Given that the bandwidth of measurement at each frequency band is 2 GHz, the delay resolution for each band is 0.5 ns, resulting in a spatial resolution is 0.15 m. The delay range of the measurement is 350 ns, which limits the maximum measurement range to approximately 105 m path length.
The measured \(S_{i}^{21}(f)\) parameter can be expressed as a product of the Tx branch, Tx antenna, the channel, the Rx branch, and the Rx antenna. The Tx branch and the Rx branch could be removed via calibration, as illustrated in Fig. 2. The antenna gains of the Tx and Rx antenna at different frequency bands are given in Table 1, and can be de-embedded in post-processing to extract the channel frequency response.
Measurement scenario
The measurements were performed in an empty room, as depicted in Fig. 3. All walls are made of concrete except the bottom wall which is a wooden board as indicated in the figure. Two scenarios were considered in the measurement: LOS and O-LOS, as shown in Figs. 4 and 5, respectively. For the O-LOS measurement, a blackboard of dimensions 1.19×1.19 m2 with one side covered by aluminum was placed between the antennas to block the paths in the LOS direction.
An illustration of the dimensions of the empty room and locations for the Tx and Rx antennas for the measurement campaign
Photograph of the line-of-sight (LOS) scenario
Photograph of the O-LOS scenario
Measurement objectives
Five objectives were targeted in the measurement campaign:
In this paper, virtual arrays (via mechanical displacement of a single Biconical antenna) and rotation of high directive horn antennas are used to investigate the power-angle-delay profiles of the indoor propagation channels. To achieve this goal, the propagation environment should be maintained static during measurement. System stability investigation was carried out in Section 4.1.
Accurate calibration of antenna element positions is required, which becomes even more challenging at millimeter wave bands. For this reason, the measurements were repeated two to three times to investigate the repeatability of the results.
Wideband channel characteristics in delay and spatial domains and room electromagnetic in the LOS and O-LOS scenarios are analyzed and compared.
One interesting research topic in millimeter wave channel modeling is the differences and similarities in channel characteristics at different frequency bands. In this paper, measured channel characteristics at 2−4, 14−16, and 28−30 GHz are compared.
Measurement results with a virtual UCA and steering horn antennas are analyzed and compared. Note that for the measurements with horns, two different horn antennas were used to cover the three frequency bands (one for 2−4 and 14−16 GHz, and the other one for 28−30 GHz), as detailed in Table 1.
Table 2 summarizes the measurement items performed in the measurement campaign.
Table 2 Measured items during the measurement campaign
Measurement results
To investigate the channel spatial profile by using a virtual array or rotating a high-directive horn antenna, it is important to ensure a static environment [16]. In order to investigate the stability of the measurement system, wideband measurements with a biconical antenna at the Rx side are performed, without rotating the turntable. That is, the channel frequency responses were repeated P=720 times for the same position of the Rx. CIRs can be calculated via inverse Fourier transform of the measured frequency responses for each frequency band. One simple way to check stability is to investigate the phase variation of the narrowband received signal, which is obtained by summing up the CIRs coherently over the delay domain. The rms phase variation of the received signal is shown in Table 3. The rms phase variation at 2−4 GHz is up to 2.9°, which is higher compared to phase variation at 14−16 and 28−30-GHz bands both for the LOS and O-LOS scenarios. This might be caused by higher instabilities in the measurements system at lower frequencies. The rms phase variations are comparable in LOS and O-LOS scenarios at all frequency bands.
Table 3 rms phase variations of the received field unit [°]
Measurements with the horn antennas and the UCA were repeated to investigate the repeatability of the measurements. Note that in this case, the turntable is rotating as shown in Table 2. To investigate the repeatability of the results, the cross correlations of the narowband received signals are calculated for each scenario among different repetitions. The cross correlation is equal to 1 when two measurement results are identical. The worst results among the repetitions are shown in Fig. 6. The measurements are generally highly repeatable, with cross correlations between repetitions above 0.98 for all scenarios. The measurements with the horn antennas are less repeatable due to a stronger cable effect (e.g., cable bending) observed in practical measurements.
Cross correlations of the received fields in two repeated measurements for different scenarios
Horn antenna results
Main path identification
The measured power-angle-delay profiles with horn antennas for the LOS and O-LOS scenarios for different frequency bands are shown in Figs. 7 and 8, respectively. The trajectories of the multipath components in the measurement room can be obtained by relating the angle and delay information of the multipaths (Figs. 7 and 8), to the room geometry (Fig. 3), as shown in Fig. 9.
Power-angle-delay profile measured with horn antennas for LOS scenarios at different frequency bands. The power dynamic range (i.e., color bar range) is limited to 35 dB. Note that the horn antenna gain is embedded in the results for all the bands
Power-angle-delay profile measured with horn antennas for O-LOS scenarios at different frequency bands. The power dynamic range (i.e. color bar range) is limited to 35 dB. Note that the horn antenna gain is embedded in the results for all the bands
Paths identified (top view) based on the results reported at 14−16 GHz and 28−30 GHz in Figs. 7 and 8 for the LOS and O-LOS scenarios. Note that path 2, which corresponds to a ground reflection, and path 3, which corresponds to a ceiling reflection, are not present in the figure
Note that the delay range is limited to 60 ns (corresponding to 18 m in distance) in Figs. 7 and 8 for illustration of the main paths. The spatial resolution is limited by the beamwidth of the horn antennas. As detailed in Table 1, the horn antenna operated at 2−4 GHz suffers from low spatial resolution both in azimuth and elevation domains, while the horn antennas operated at 14−16 and 28−30 GHz are much more directional, with a beamwidth of 20° at the 28−30 GHz band in azimuth domains. The delay resolution, however, is the same, since the same bandwidth is set for the three frequency bands.
LOS measurements at different frequency bands are dominated by the LOS paths, while the O-LOS measurement is more spatially rich, with quite a few dominant paths in various specular directions. As seen in Figs. 7 and 8, multipath components identified in the LOS and O-LOS scenarios are quite similar, except the paths impinging the Rx with AoAs around 0o and 180o, which are blocked by the blackboard. It is worth noting that these paths have a slightly different interpretation in the LOS and O-LOS cases. For example, the path identified as 1 has the same AoA for both cases, yet it corresponds to the LOS in Fig. 7, whereas in Fig. 8 it corresponds to a diffracted path from the top edge of the obstructor. The radius of the nth Fresnel zone can be calculated as:
$$ F_{n} = \sqrt{\frac{n \lambda d_{1} d_{2}}{d_{1} + d_{2}}}, $$
where d 1, d 2 is the distance from the obstructor to the Tx and Rx, respectively. In our measurement, the radius of the first Fresnel zone at 30 GHz is 0.11 m, whereas the height difference between the blackboard and the antennas is only 0.09 m; thus the first Fresnel zone was not completely obstructed by the blackboard, resulting in the diffraction identified as path 1 in Fig. 8. The power angle spectra measured for the LOS and O-LOS scenarios at 14−16 and 28−30-GHz frequency bands are shown in Fig. 10. The power angle spectra in the LOS scenario match quite well with those in the O-LOS scenario in non-LOS directions for both frequency bands, as expected.
Power angle spectra measured for the LOS and O-LOS scenarios at 14−16 and 28−30-GHz frequency bands. Note the power values at two different bands are normalized to the LOS component at 14−16 and 28−30 GHz, respectively
Contrary to the fact that only a few specular paths are identified at 14−16 and 28−30 GHz, measured channels at 2−4 GHz present quite different results. This observation is consistent with results published in the literature, i.e., channel profiles at millimeter wave bands are characterized by fewer and sparser dominant paths compared to typical cellular bands [9, 10]. A richer multipath environment can be observed for the results at 2−4 GHz, with many more paths present in the delay domain. This might be due to a stronger diffuse scattering from objects at the low frequency band, as the wavelength is more comparable to object dimensions at the low frequency. At the higher bands, the wavelength is much smaller, and hence specular reflections are dominant. Different dominant paths can be identified at 2−4 GHz. Although some specular paths can be identified at all frequencies (e.g., path 1, 2, 3, 4, 5, and 6), some of the paths present at 2−4 GHz can not be identified at higher frequency bands (e.g., path 11 and 12). Also, some specular paths present at high bands (e.g., path 7 and 8) cannot be clearly identified at the low frequency band.
The main propagation paths from the Tx to the Rx can be identified, as shown in Fig. 9. The angles and delays of the identified paths at 14−16 and 28−30 GHz are quite similar both for the LOS and O-LOS scenarios. However, the normalized power values of the identified paths with same delay and angle at different frequency bands might be different. As shown in Fig. 10, although main paths impinge the Rx at same angles, the power values are different.
In [2], scattering effects are shown in the measurements, whereas only specular components can be seen in our measurements at 28–30 GHz. This might be due to the fact that a small furnished office, where small scatterers exist, was investigated in [2], whereas an empty room with a few scatterers was selected in this paper. Moreover, a wide dynamic range was used in [2], whereas in this paper, the dynamic range in this paper is limited to 35 dB in order to investigate only the dominant components. A richer multipath environment could be expected in a furnished room as shown in [16].
Room electromagnetic
Discussions in section 4.3.1 were focused on the accurate characterizations of the main propagation paths, i.e., the LOS path and main reflected paths from the walls and ground. We are also interested in the remaining part of the CIRs that correspond to the non-dominant paths. The rms delay spread τ rms and mean excess delay \(\bar {\tau }\) are often calculated with respect to a threshold relative to the strongest path. This ensures full compatibility of the results, since noise is excluded from the calculation. The τ rms and \(\bar {\tau }\) using a 30 dB threshold are shown in Table 4 for the LOS and O-LOS scenarios at different frequency bands. τ rms and \(\bar {\tau }\) are larger in the O-LOS scenarios compared with the LOS scenarios for all frequency bands as expected, with an exception that τ rms in the O-LOS scenario is slightly smaller at 2−4 GHz, compared to the higher frequency bands. τ rms and \(\bar {\tau }\) at 2−4 GHz in the LOS scenario are larger compared to higher frequencies due to the richer multipath environments at the low band. τ rms and \(\bar {\tau }\) at the O-LOS scenarios are, however, comparable at the three different frequency bands.
Table 4 τ rms and \(\bar {\tau }\) for the LOS and O-LOS scenarios at different frequency bands
The tail of the power delay profiles (PDPs) generally have exponential decays with approximately the same decay rates for different scenarios at different frequency bands, as shown in Table 4, with a deviation up to 0.02 dB/ns around −0.26 dB/ns decay rate. The decay rate of the delay tail is governed by the overall dimensions of the room and an average absorption coefficient, and it is irrelevant to the propagation scenarios (i.e., LOS or O-LOS) [18]. This is due to the fact that the room will be filled with energy, resulting in a constant energy density for the same delay [18]. It can be concluded based on the measurement results that the average absorption coefficient does not depend on frequency. Note that the decay rates were calculated based on CIRs ranged from 60 to 200 ns to avoid including the dominant paths. If the CIRs before 60 ns, where dominant paths are present, are considered, the calculated decay rate will be different. The PDPs for the LOS and O-LOS scenarios at 28−30 GHz and the fitted lines are shown in Fig. 11. Note that different scenarios at different frequencies not only have the delay tails with the same decay rates, but also the power values in tails are the same as well, as shown in Fig. 11.
Average power delay profiles for the LOS and O-LOS scenarios at 28−30 GHz. Kaiser window with β=6 was applied to suppress the sidelobes in the inverse Fourier transform
UCA measurement results
Path loss
For the virtual UCA measurements, the path loss at each element position i at each frequency band can be expressed as:
$$ PL(i)=\frac{1}{N}\sum\limits_{n=1}^{N}|H_{i}(f_{n})|^{2}. $$
The path loss results for the LOS and O-LOS scenarios for the three frequency bands are shown in Fig. 12. In the LOS scenario, the measured path loss results match well with the calculated path loss from Friis equation, as the LOS path is dominant. The deviation is mainly due to the inaccurate antenna gains provided in Table 1 for different frequency bands. The ripples in the measured results are caused by the paths from non-LOS directions. The path loss in the LOS scenario varies along element positions as expected, e.g., minimum path loss present at element position 360 (i.e., orientation angle 180°), which corresponds well to the element positions illustrated in Fig. 3. The path loss in O-LOS scenario is around 10 dB higher compared to LOS scenario for 14−16 and 28−30-GHz bands, while only around 4 dB higher for 2−4 GHz.
Path loss over different array element positions for three frequency bands for the LOS and O-LOS scenarios. Note that the transmit and receive antenna gains at different frequency bands are de-embeded from the results
Power-angle-delay profile
The CIRs received at different UCA element positions for the LOS scenario at different frequency bands are shown in Fig. 13. Similar to horn antenna measurement results, a richer multipath environment can be observed at 2−4 GHz, compared with higher frequency bands. Only a few specular paths can be identified from the delay variation along array element positions at 14−16 and 28−30 GHz.
CIRs recorded at different UCA element positions for the LOS scenario at different frequency bands
The power-angle-delay profiles obtained with frequency beamforming techniques discussed in Section 2 for the LOS and O-LOS scenarios at different frequency bands are shown in Figs. 14 and 15, respectively. Similar to the horn antenna measurement results, richer multipath environments can be observed at 2−4 GHz, compared to results in high frequency bands, both for the LOS and O-LOS scenarios. Similar power-angle-delay profiles are present at 14 – 16 and 28 – 30-GHz frequency bands. A few dominant specular paths can be identified for all the frequency bands. Compared with horn antenna results in Figs. 7 and 8, paths with same impinging angles and delays are observed both for the LOS and O-LOS scenarios at different the frequency bands. The measured power-angle-delay profiles with the UCA, although with higher spatial resolution, suffers from high side lobes as well. As explained in [24], the joint sidelobes in delay and angle domains are caused by the joint frequency and angle dependance inherent in phase in Eq. (4) with the conventional beamforming technique. The focus of future work will be on resolving the multipath components from the array measurement results with other techniques, e.g., frequency invariant beamforming technique [24].
Power-angle-delay profile measured with UCA for LOS scenarios at different frequency bands. The power dynamic range is limited to 35 dB
Power-angle-delay profile measured with UCA for O-LOS scenarios at different frequency bands. The power dynamic range is limited to 30 dB
This work presents an extensive measurement campaign and a detailed analysis of spatial-temporal channels at centimetric and millimetric bands in an indoor environment. Multipath components were resolved in space and delay via steering a wideband horn antenna and via measurements with a virtual wideband UCA in different frequency bands, respectively. Measurement results include stability levels, repetition levels, power-angle-delay profiles, path loss, room electromagnetic, etc. Results show that:
The measurement system is quite stable, with a rms phase drift up to 1.5° at 28−30 GHz band.
The measurement results are highly repeatable, with a correlation between two repeated measurements up to 0.98.
Richer multipath components are present at lower frequency bands due to diffuse scattering effects, while specular reflections are dominant at millimeter wave bands. The trajectory of the specular components in a room are identified by relating the multipath angle and delay information to the room geometry. Investigations in a furnished room, where more scatterers exists, will be performed in future work.
Room electromagnetics are not frequency dependent in an empty indoor scenario. The tails of the PDPs can be modeled with a exponential decay with decay rate around −0.25 dB/ns.
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This work has been supported by the Danish High Technology Foundation via the VIRTUOSO project. The authors appreciate the assistance from Kristian Bank and Yi Tan with the practical measurements. The authors would like to thank Dr. Lishuai Jing and Dr. Ming Shen for the active discussions.
Department of Electronic Systems, Faculty of Engineering and Science, Aalborg University, Aalborg, Denmark
Wei Fan
, Ines Carton
, Jesper Ø. Nielsen
, Kim Olesen
& Gert F. Pedersen
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Correspondence to Wei Fan.
Fan, W., Carton, I., Nielsen, J.Ø. et al. Measured wideband characteristics of indoor channels at centimetric and millimetric bands. J Wireless Com Network 2016, 58 (2016). https://doi.org/10.1186/s13638-016-0548-x
DOI: https://doi.org/10.1186/s13638-016-0548-x
Millimeter wave channel measurements
Spatio-temporal channel modeling
Room electromagnetics
Angle of arrival estimation
Radio Channel models for higher frequency bands


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According to the Hill, many insurance companies are contradicting HHS Secretary Sebelius's rosy predictions about modest increases in Obamacare premiums next year.
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How long is this "Breaking News" going to be featured? The article was written in March, 2014, and, as we now know, is completely off the mark. I just finished Googling another "Breaking News" article written by Michael Chandler in 2013 which was equally inaccurate in its predictions. Are you lacking for current content?