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Justia Dockets & Filings Sixth Circuit Tennessee Middle District Large v. Blazer Filing 54
Large v. Blazer
MEMORANDUM OPINION AND ORDER OF THE COURT: Plaintiff's motion to compel 44 is denied. Further, Defendant's request for a protective order is granted and the requested documents need not be produced. Signed by Magistrate Judge Barbara D. Holmes on 1/10/2022. (DOCKET TEXT SUMMARY ONLY-ATTORNEYS MUST OPEN THE PDF AND READ THE ORDER.)(kc)
IN THE UNITED STATES DISTRICT COURT FOR THE MIDDLE DISTRICT OF TENNESSEE TERESA LARGE, as surviving wife and on behalf of the decedent, NICK LARGE v. DR. DAVID BLAZER ) ) ) ) ) ) Case No. 3:20-cv-1012 Chief Judge Crenshaw Magistrate Judge Holmes MEMORANDUM OPINION AND ORDER Pending before the Court is Plaintiff's motion to compel discovery from a nonparty, State Volunteer Mutual Insurance Company ("SVMIC") (Docket No. 44) ) and SVMIC's response in opposition. (Docket No. 52.) The same issues are addressed in the parties' joint discovery dispute statement. (Docket Nos. 43 and 46.) For the reasons discussed below, Plaintiff's motion (Docket No. 44) is denied and Defendant's request for a protective order is granted. I. Background Familiarity with this case is presumed and the underlying facts and procedural history are recited here only as necessary to explain or provide context to the Court's ruling.1 This healthcare liability action, over which the Court has diversity jurisdiction, arises out of the care and treatment of Nick Large in March of 2020. Plaintiff alleges that Defendant negligently performed a cardiac catheterization and provided negligent follow-up care for Mr. Large, which ultimately resulted in his death. By the instant motion to compel, Plaintiff seeks to enforce a subpoena issued to non-party, SVMIC, which is Defendant's professional liability insurance carrier. On November 5, 2021, shortly after being served with Defendant's disclosures of retained experts, Plaintiff served the 1 The facts and procedural history are taken from the record in this case and, unless otherwise noted, are generally undisputed. Case 3:20-cv-01012 Document 54 Filed 01/10/22 Page 1 of 8 PageID #: 336 subpoena requesting: (i) an authenticated copy of a document already produced by SVMIC and (ii) documentation regarding whether Defendant, Defendant's retained experts, and two additional physicians who were treatment providers for Nick Large, and who were identified in Rule 26(a) initial disclosures by Defendant, are "(a) insured with SVMIC and (b) whether they have received a dividend from SVMIC and/or are so eligible." (Docket No. 44 at 2.) SVMIC agreed to provide an authenticated copy of the subject document and appears to have provided that copy on December 10, 2021. (Docket No. 52 at 2.) SVMIC objects to the additional request based on the lack of any temporal limitation and the vagueness and breadth of the request, and because the request implicates private and privileged information. (Id. at 2-6.) For the reasons discussed below, the Court finds the motion to compel is without merit and is therefore denied. Further, the Court finds good cause for a protective order under Rule 26(c). II. Legal Standards Rule 45 of the Federal Rules of Civil Procedure governs third-party subpoenas. It permits parties to a lawsuit to command a non-party to, among other things, produce documents. Fed. R. Civ. P. 45(a)(1). A court is required to quash or modify a subpoena that "requires disclosure of privileged or other protected matter, if no exception or waiver applies" or "subjects a person to undue burden." Fed. R. Civ. P. 45(d)(3)(A). The scope of discovery under a subpoena is the same as the scope of discovery under Rule 26. Fed. R. Civ. P. 45, Advisory Committee Notes (1970) ("The scope of discovery through a subpoena is the same as that applicable to Rule 34 and the other discovery rules."); see also Hendricks v Total Quality Logistics, LLC, 275 F.R.D. 251, 253 (S.D. Ohio May 6, 2011). The party seeking to quash a subpoena bears the burden of proof. Id. The Federal Rules of Civil 2 Case 3:20-cv-01012 Document 54 Filed 01/10/22 Page 2 of 8 PageID #: 337 Procedure grant parties the right to "obtain discovery regarding any nonprivileged matter that is relevant to any party's claim or defense and proportional to the needs of the case." Fed. R. Civ. P. 26(b)(1). A trial court has broad discretion to determine the proper scope of discovery. In re Ohio Execution Protocol Litigation, 845 F.3d 231, 236 (6th Cir. 2016). Although a party should not be denied access to information necessary to prove their contentions, neither should they be "permitted to go fishing and a trial court retains discretion to determine that a discovery request is too broad and oppressive." Id. (internal citation omitted). "A court must balance the "right to discovery with the need to prevent fishing expeditions." Id. at 236-37 (internal quotation marks and citation omitted). The proponent of a motion to compel discovery bears the initial burden of proving that the information sought is relevant. O'Malley v. NaphCare Inc., 311 F.R.D. 461, 463 (S.D. Ohio 2015) (internal quotations and citations omitted). See also Grae v. Corr. Corp. of Am., 326 F.R.D. 482, 485 (M.D. Tenn. 2018) ("The court will only grant [a motion to compel], however, if the movant actually has a right to the discovery requested.") When the information sought appears to be relevant, the party resisting production has the burden of establishing that the information either is not relevant or is so marginally relevant that the presumption of broad disclosure is outweighed by the potential for undue burden or harm. O'Malley v. NaphCare Inc., 311 F.R.D. at 463. Rule 26(c) provides that "[t]he court may, for good cause, issue an order to protect a party or person from annoyance, embarrassment, oppression, or undue burden or expense." Fed. R. Civ. P. 26(c). Courts within the Sixth Circuit have interpreted Rule 26(c) to permit a party to seek a protective order to preclude discovery demanded by a third-party subpoena. Schweinfurth v. Motorola, Inc., 2008 WL 4981380, at *2 (N.D. Ohio Nov. 19, 2008) (citations omitted). Some courts have referred to the availability of Rule 26(c) as "standing to challenge third-party 3 Case 3:20-cv-01012 Document 54 Filed 01/10/22 Page 3 of 8 PageID #: 338 subpoenas via a motion for protective order." Id. at *3.2 "The burden of establishing good cause for a protective order rests with the movant." Nix v. Sword, 11 F.App'x. 498, 500 (6th Cir. 2001) (internal citations omitted). However, a showing of irrelevancy of proposed discovery can satisfy the good cause requirement of Rule 26(c). Anwar v. Dow Chemical Company, 876 F.3d 841, 854 (citing Smith v. Dowson, 158 F.R.D. 138, 140 (D.Minn.1994)). Ultimately, whether to grant a protective order is within the discretion of the trial court. Coleman v. American Red Cross, 979 F.2d 1135, 1138 (6th Cir. 1992). III. Analysis Plaintiff seeks information from SVMIC about Defendant, four experts retained by Defendant – Drs. Crenshaw, Stankewicz, Bresee, and Souther – and two physicians who were treating providers of the decedent – Drs. Alsoub and Goodman. Plaintiff's theory is essentially that, if the six other physicians are also insured by SVMIC, as is Defendant, that information goes to their potential bias because of their insured relationship, described by Plaintiff as one of coownership with Defendant, and the possibility of dividends based on SVMIC's financial performance, which may be impacted by the outcome of this lawsuit. See Docket No. 42 at 8-9. However, rather than deposing any of the physicians to determine if they are, in fact, insured by SVMIC and, if so, whether they have received dividends or even understand the dividend structure, Plaintiff instead elected to subpoena the information from SVMIC, who is not a party to this litigation. Plaintiff did so without knowledge of whether any of the other physicians are insured by SVMIC and based solely on the supposition that if they are SVMIC insureds, they 2 Although no separate motion for a protective order was filed, Defendant requested that relief in the joint discovery dispute statement. (Docket No. 42 at 5.) As provided for in the initial case management order, the filing of a discovery motion is within the discretion of the Court. Here, the Court finds that the parties' positions are aptly described in the joint discovery dispute statement and the filing of a separate motion for protective order is unnecessary. 4 Case 3:20-cv-01012 Document 54 Filed 01/10/22 Page 4 of 8 PageID #: 339 will receive some dividend that may be impacted in some unknown and undescribed way by the outcome of the case against Defendant. This is a classic fishing expedition. While it is correct that some discovery from experts to evaluate their bias may be permitted, Plaintiff does not contend that she is lacking in the kind of information about the retained experts from which bias is ordinarily evaluated, such as their hourly rate in this case or their previous testimony as defense experts generally or on behalf of Defendant specifically.3 See e.g. Campos v. MTD Products, Inc., No. 2:07-00029, 2009 WL 920337, at *4 (M.D. Tenn. Apr. 1, 2009) (routine disclosure of an expert's gross compensation from all sources, including those unrelated to the litigation is overkill and permitted only upon showing that other information is insufficient to evaluate bias). Nor has Plaintiff presented any facts supporting her theory of bias or lack of objectivity in this case. Rather, Plaintiff has simply thrown out a line in hopes that she can reel in information to fill her bias creel. She does not assert, for instance, that the other physicians are insured by SVMIC or that even if insured by SVMIC and potential recipients of dividends, those experts have a direct financial connection to this case that would be relevant to proving bias toward or against a particular party. Plaintiff merely supposes that the SVMIC dividends are structured in such a way that an outcome favorable to Plaintiff would impact dividends paid to other locally insured physicians, including the experts, if insured by SVMIC, in Although the specific expert disclosures were not filed as part of the record, it is the Court's understanding from the informal discovery conference that detailed information about the experts was produced in accordance with Rule 26(a)(2)(B). Further, and more importantly, Plaintiff had knowledge of the two treating physicians, presumably based on her own information, and, if not, through Defendant's initial disclosures that were made in or around February of 2021. If Plaintiff believed there was some direct relationship between the physicians and Defendant through SVMIC or otherwise that demonstrates bias, she could have deposed those treating physicians at any earlier time. She could also have deposed the physicians designated as experts to elicit their testimony about the insured status with SVMIC and their knowledge of any dividend structure before issuance of the subject subpoena. 3 5 Case 3:20-cv-01012 Document 54 Filed 01/10/22 Page 5 of 8 PageID #: 340 an amount that would influence them to testify favorably to Defendant. This is a purely speculative and tenuous supposition based on general, public statements made by SVMIC. The Court finds persuasive the careful analysis in Langbord v. U.S. Dept. of Treasury on the question of discovery about an expert's indirect relationship to the litigation. Civil Action No. 06-CV-05315, 2008 WL 4748174 (E.D. Penn. Oct. 22, 2008). As noted in Langbord, even if certain information is relevant to show potential bias, "the simple fact that requested information is discoverable ... does not mean that discovery must be had." Nicholas v. Wyndham Intern., Inc., 373 F.3d 537, 543 (4th Cir.2004). Under Rule 26(b)(2)(C), a court must limit discovery if "the burden or expense of the proposed discovery outweighs its likely benefit, considering the needs of the case, the amount in controversy, the parties' resources, the importance of the issues at stake in the action, and the importance of the discovery in resolving the issues." In fact, in its comments to the 2000 amendments to Rule 26, the Rules Advisory Committee stated, "The Committee has been told repeatedly that courts have not implemented [the Rule 26(b) (2)] limitations with the vigor that was contemplated ... [the new language] has been added to emphasize the need for active judicial use of subdivision (b)(2) to control excessive discovery." Advisory Committee's Note to the 2000 Amendments to the Federal Rules of Civil Procedure. The Supreme Court has also highlighted the importance of Rule 26(b)(2), emphasizing that the rule gives courts "broad discretion to tailor discovery narrowly." Crawford-El v. Britton, 523 U.S. 574, 598, 118 S.Ct. 1584, 140 L.Ed.2d 759 (1998). In the foregoing analysis, we exercise that discretion by applying the balancing test of Rule 26(b)(2)(C)(iii) to the benefits and burdens presented by the proposed discovery. Id. at *5. Here, as in Langbord, Plaintiff's theory that the experts may be biased because an outcome in favor of Plaintiff in this litigation could potentially affect some dividend they might receive from an insurance company with which they may not even be insured is nothing more than unsubstantiated speculation. The fact that the information requested relates to individuals who are not parties to this matter and the fact that the request is based on purely speculative grounds "points against a finding that the discovery is highly necessary or important for uncovering bias in this matter." Id. at *6.4 Further, even if the physicians are insured with SVMIC and even if they do receive some dividend, a finding of need for and importance of the proposed discovery to show bias, supposes 4 6 Case 3:20-cv-01012 Document 54 Filed 01/10/22 Page 6 of 8 PageID #: 341 In contrast, the burden to SVMIC is substantial. It would require disclosure of confidential and proprietary information about SVMIC's business and financial structure and, potentially (that is, to the extent any of the expert physicians are insured with SVMIC), disclosure of customers' confidential and personal financial information. Permitting Plaintiff to access SVMIC's and its customers' confidential and sensitive proprietary and financial information unrelated to this action based on solely unsupported speculation is unwarranted. "Although a plaintiff should not be denied access to information necessary to support her claim, neither may a plaintiff be permitted to 'go fishing' and a trial court retains discretion to determine that a discovery request is too broad or oppressive." Surles v. Greyhound Lines, Inc., 474 F.3d 288, 305 (6th Cir. 2007) (citing Marshall v Westinghouse Elec. Corp., 574 F.2d 588, 592 (5th Cir. 1978)) (internal quotations omitted). The significant burden on SVMIC's proprietary and confidential business and customer information unrelated to this litigation or to the physicians' role as expert witnesses weighs heavily against allowing the requested discovery under Rule 26(b)(2)(C)(iii). Because the discovery request places a significant burden on SVMIC and because the requested information is not sufficiently important or necessary to outweigh that burden, Rule 26(b)(2)(C)(iii) bars Plaintiff's request to compel the discovery and warrants a protective order under Rule 26(c). that the expert physicians possess an understanding of the intricacies of their insurance dividend structure with enough detail to influence their opinions, which is yet another factual leap the Court is unwilling make. 7 Case 3:20-cv-01012 Document 54 Filed 01/10/22 Page 7 of 8 PageID #: 342 IV. Conclusion For these reasons, Plaintiff's motion to compel (Docket No. 44) is denied. Further, Defendant's request for a protective order is granted and the requested documents need not be produced. It is SO ORDERED. ______________________________________ BARBARA D. HOLMES United States Magistrate Judge 8 Case 3:20-cv-01012 Document 54 Filed 01/10/22 Page 8 of 8 PageID #: 343


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Author: Cameron Milne
Polished but Not Finished
December 20, 2017 January 2, 2018 Cameron Milne	Gateway Manis F17	Leave a comment
This blog post is dedicated to my Eportfolio that while is not finished, is ready to be seen. The website features a landing page of downtown Des Moines, Iowa, where I interned this past summer. Throughout the website, one can find my works of trying to summarize the experience in three separate genre experiments, each producing a new perspective than the others. It was through these experimentations that I learned how much one mode of communication can vary from another. While my immersive journalism piece offered a detailed look into the office of a company, a short film screenplay was able to show audiences information that would have been potentially rude to write about.
This semester has offered me a chance to explore my own summer experience by interacting with different genres and mediums of expression. Each afforded me the ability to tell the story in a powerful way due to the conventions of that genre. They also, however, limited my message in some way due to the very same reason. This push and pull situation forced me as a writer (and reader) to consider in depth the rhetorical choices I made when experimenting.
Take a look at my website if you get a chance. I would like to personally thank whatever database gave me the old pictures of Des Moines through Google images.
https://cmilne11.wixsite.com/gatewayeportfolio
Writer to Writer: Howard Markel
November 21, 2017 November 28, 2017 Cameron Milne	Gateway Manis F17	Leave a comment
On Tuesday, November 21st, I attended the Writer to Writer Series featuring the accomplished medical history writer, Howard Markel. The event, moderated by the brilliant, feared Shelley Manis, began with an introduction of Howard Markel, followed by a series of questions on his current work and writing processes. The event ended with a few rapid fire questions (which writers would you like to bring to a writing retreat?, etc.) and a Q/A session with the audience.
Howard Markel is downright impressive. Next to him, calling myself a writer doesn't feel appropriate. After majoring in English as an undergraduate, he went on to receive an M.D. from the University of Michigan Medical School and then a Ph.D. at the John Hopkins University. Beyond the 10+ years in school, his writing accomplishments include self-authoring or coauthoring ten books, 12 years of writing for the New York Times, monthly medical history writings for NPR and the American Journal of Public Health. On top of his "1000 words" he writes daily, he teaches at the University of Michigan. Fun fact, as a teenager, he was paid $5 per joke he wrote for The Detroit News.
He had much to say on the topic of today's writers and what it means to be a flexible rhetor. Howard prefers to complete his daily writing in his pajamas whilst listening to Mozart– Beethoven is "too intellectual." When asked what's wrong with today's writing, he mentioned the need writers feel to solicit themselves in their work. Respectfully, I disagree Howard, but that's irrelevant. At the end of the session, he made a statement that made the entire event worthwhile…"Regardless of how bad the times are or how frustrated we are with something, we have the opportunity to write about it." This statement deserves its own space on a plaque or maybe a feature on some avant garde film. Either way, I'm skeptical that he was the first one to say it.
Howard was delightful to listen to and seemed to understand his audience perfectly–a learning objective for the minor in writing students. He discussed his experiences of writing for an audience of nine people versus a million. The audience he writes for shapes the genre and style of writing he produces. Howard's consciousness of his own writing lends itself to a variety of intended outcomes that other writers may never achieve.
An Ode to The Office
October 30, 2017 October 30, 2017 Cameron Milne	Gateway Manis F17	Leave a comment
The Proposal: Short Film Mockumentaries
Social media content is becoming increasingly more visual in today's world. I scrolled down my Facebook timeline today and those lengthy blog posts that were more prevalent a few years ago have been replaced with videos and photos. The content we see on social media is a direct response to how people want their information and the formats that are effective in conveying information. Why read an article when you can look at an infographic or watch a commentary on an event and gain the same information quicker? When we passively take in information, visual channels seem to be the most effective in underscoring the intended message. For my third experiment, I will write a script for a short film mockumentary on a day in the life of Dull, Inc. To placate the masses, I need to transform the original piece into a genre that will utilize specific elements of film to connect with audiences.
The rhetorical situation is an internship experience in Des Moines, Iowa, working for a multifamily real estate management company. The experience was filled with plenty of frustrations, comical observations and important takeaways for myself that I have decided to explore through writing experiments.
The rhetorical purpose for my short film is to give my audiences a perspective on the topic that they wouldn't otherwise understand had the short film been replaced by another format. Because the purpose of film is to capitalize on the specific elements afforded by visual storytelling that enhance a story in ways that traditional writing cannot, my short film will take full advantage of the surroundings, context, and other visual information that could be better shown than described to display the frustration of feeling out of context.
The primary audience for my short film mockumentary will be employers, bosses, leaders and other authoritative figures in work environments that have the power to affect change. Invoked audiences can be the employees that feel trapped or unsatisfied, interns that have dealt with similar experiences or teenagers curious about what it means to work in a typical office.
The conversation I'm hoping to join is on office life and the frustrations of the underutilized worker. A short film mockumentary done right could be the doorway for pulling many others into the conversation that grow stronger with size. With the right momentum, the authoritative figures in offices, companies and work environments can be shown a perspective outside of their own on a culture they are responsible for. If I can connect with others on those frustrations of office life and sway them to view something about their own work, the potential for change will have increased tenfold.
How to Write a Short Film Mockumentary
An introduction to the short film script.
The short film is particularly effective for telling stories because of its brevity and ability to convey a message. In a matter of minutes, a short film can engage any viewer emotionally through a compelling story that has established stakes, conflict to be resolved and internal or external dilemmas. They serve as the perfect vehicle for demonstrating an idea or concept to audiences in an entertaining format because visual storytelling has the power to convey emotion, which is highly effective in educating audiences on concepts. Rather than write an article on the courage taken by gay teenageers that come out to their friends and peers, a short film could capture every moment of emotion in their journey can give audiences the opportunity to empathize and understand with a foreign concept (In a Heartbeat – Animated Short Film). Below are some requirements for the short film mockumentary.
1. Short Film means Short
At most, short films can be 50 minutes as determine by the Sundance Film Festival. The rule of thumb for screenwriting is the amount of pages will be the length in time of the film. Thus, screenwriters typically cap their screenplays at 120 pages because it reads as a two hour film. Shorter is better when creating short films for the sake of mathematics. If a festival is forced to choose between two ten minute short films in place of a twenty minute short film for programming, they will opt for the two shorter films (No Film School).
2. Brevity and Density
The short film only has minutes to convey the intended message and therefore the filmmaker has to quickly establish goals or stakes that help to develop the character(s) and keep the audience interested. If a twenty minute short film can be condensed into a ten minute short film, the filmmaker should proceed to cut out anything that isn't vital for the story or the intended impact. This is one of the major drawbacks of short films because it is so challenging to cut irrelevant moments or Because short films have the reputation of addressing the point quickly, audiences allow themselves to be pulled in knowing it will be over soon unlike longer films that discourage viewers for their lengthy run times. Viewers know that a point will be made, a goal will be achieved, an internal conflict solved or some other problem fixed in a matter of minutes and thus they are willing to stick with it longer.
2. The Mockumentary
I spent a lot of time watching The Office to better understand this genre. The tv show aired on NBC and won several Emmy's for its writing, serving as the example for all sitcoms and mockumentary style films. The show portrays a typical office and its employees in their daily lives, but pairs this with endless comedy that becomes addicting to watch. While the show is not classified as a mockumentary, there are elements of the of the documentary-style sitcom that closely resemble a mockumentary.
A mockumentary can be defined as a motion picture or television program that takes the form of a serious documentary in order to satirize its subject (Wikipedia). The Office's unique approach consists intercutting between scenes that display real-time events occuring and interview scenes giving their opinions in hindsight that affords the filmmaker the opportunity to create an entertaining narrative effective for comedic purposes. What's specific to a documentary or mockumentary are the way scenes are composed through camera angles. The Office pairs scenes of objective shots (observing a scene from the outside) in which the camera appears to be hidden with interviews where characters break the fourth wall by speaking directly to a camera. A motion picture that is classified as a mockumentary will consist of these types of scenes.
3. A Specific Type of Comedy: Satire
The Office appeals to mass audiences because of their specific approach to humor. When asked how the show's writer, Brent Forrester, approaches each episode, he responded saying "silly isn't funny" (Vanity Fair). He went on to discuss how the real funny stuff comes from tragedy, but there exists a fine line between comedy and tragedy. Some stuff is inappropriate to be laughing at but "stuff that's a little bit difficult–that's where humor really lies." A mockumentary lands well when it pokes fun at some aspect of culture or society where a deeper flaw lies beneath the surface–this is satirical humor.
Satire can be defined as the use of humor, irony, exaggeration, or ridicule to expose and criticize people's stupidity or vices (Wikipedia). When a motion picture appears to be taking whatever issue that's at stake unseriously, the audience naturally leans forward in their seats, curious to why they are 'mocking' the problem. Consequently, the mockumentary is successful because its humor is effective in pointing that flaw out to the audience.
A Proposal and Guide for Writing Immersive Journalism like David Foster Wallace
October 8, 2017 October 8, 2017 Cameron Milne	Gateway Manis F17	1 Comment
My high school english classes were the most interesting classes in my IB program. This was largely due to some awakening I experienced in writing and reading thanks to a man known as David Foster Wallace. Our first assignment was to analyze and comment on the choices made by the writer David Foster Wallace in his essay "Consider the Lobster." In his article, DFW shared his experiences of attending the annual Maine Lobster Festival that included observations of its attendees, a history of lobster catching, and a philosophical exploration of whether lobsters feel pain when being boiled alive. It may seem underwhelming but his writing is addictive.
DFW reflecting on his intelligence in all matters unrelated to fashion
DFW has written many articles over his lifetime for small magazine publications or news media websites, but unlike other writers, DFW's work stands head and shoulders above his peers for its ingenuity and brilliance. Not only does he engage mundane topics in ways that are disruptive to how we view things, he does so while unapologetically bashing their existence and succeeding in leading us as readers to question it too. Reading his work opened my eyes to a style of writing that felt scandalous relative to the academic writing I had been familiar with prior to the class. He engages topics that are overlooked or under considered in ways that are endlessly entertaining–leading me to want to emulate this approach to immersive journalism.
Immersive journalism is the appropriate genre for someone who wants to write about their experiences in their summer internship working real-estate finance in Des Moine, Iowa. I currently possess a list of observations and opinions that are begging to be written for audiences that can emphasize with my trauma of corporate boredom. Immersive journalism is a form of news reporting or in my case, informative writing, that's written by someone who has experienced that subject matter personally. Because the topic of my writing will be on the mind-numbingly boring life of Iowa real estate finance, a style of writing similar to DFW's will help me entertain my audiences while informing them of what that life is like.
Immersive journalism will allow me to be effective in sharing my experiences for a few reasons. It's affords me the opportunity to foster empathy in my audience by sharing personal experiences as opposed to a commentary on office life from someone on the outside looking in. Because I am joining several conversations on corporate life, Iowa life, intern life, and boredom life, immersive journalism will allow me to serve the purpose of my genre: to inform while entertaining. I mention entertain because this is not some article on sex trafficking in Nigeria. I am going to attack the boredom of working in Iowa for a company with an average employee age between 45 and 55. This will not be a serious matter and because my complaints will most certainly come off as petulant, they will be complemented with humor targeted at myself.
Lastly, my piece would preferably be published in an independent magazine. Because the final product would be too long for a new source like NYT or the Washington Post, It would be more appropriate for a magazine, intended for laid back readers with the time for a more sizable chunk of reading. The audience is nobody in particular, but can be anyone subscribed to that magazine and are hooked by the title of the article. The goal is to entertain as many people as possible and because the article will touch on topics that are felt by those working in environments that are slow or regressive, they will be the audience I hope to reach.
The following are a list of elements that are necessary in defining my self-titled genre I will explore for experiment two: David Foster Wallace Immersive Journalism.
1.Immersive Journalism is told in first person about the events or situations experienced by that writer.
Immersive journalism is when a journalist immerses their self into the experience of which they're writing about in order to provide more depth and insight in their work. While the write does not necessarily have to express their thoughts on certain moments or aspects of that experience, the narrative will ultimately take on the first person perspective. The first person narrative is particularly effective in this genre for it's ability to create empathy in its audience. Immersive journalism when utilizing empathy has the power to convey information that may otherwise be difficult without someone who has experienced it themselves.
2. Journalism in itself is the profession of writing for the sake of news and therefore the primary goal is to inform.
Journalism is defined by the American Press Institute as the "activity of gathering, assessing, creating, and presenting news and information. What distinguishes journalism as a whole from any other genre of writing is that it's centered on news. It's rhetorical purpose is to inform the audience on something of relevance in a way that caters to their needs. By needs, I mean how that reporting is delivered to the audience for their ease, appealing to their emotion when appropriate and including evidence that maintains their curiosity in the subject matter.
3. The "David Foster Wallace" part of the genre title infers a style of immersive journalism that extends beyond basic reporting of news.
The reason I have chose this genre is not for the immersive journalism component, but because of the way David Foster Wallace composed his immersive journalism. His style of writing is unique from any other kind of immersive journalism and it is one I will attempt (and probably fail) to emulate. For those who have been living in caves, David Foster Wallace is considered one of the greatest writers of the twenty first century. Having blown the minds of self aware teenagers and mature adults everywhere, his style of writing is what journalism should strive to be: form-breaking and entertaining while fact-based and brutally honest. On writing, DFW was quoted saying "If a writer does his job right, what he basically does is remind the reader of how smart they are. Wake the reader up to stuff that reader's been aware of all the time." This is clear in his work as he has made a name for bashing the most mundane events, qualities, and situations in our culture. He has contributed a perspective to topics that can make anyone become addicted to learning more. However, he's not to be mistaken as someone who only sneers at the behavior of others as the "primary butt of [his] humor is himself" (NYT). His creative approach to immersive journalism will be the style of writing I attempt to emulate.
4. Undefined Writing Structure
There aren't any conventions that apply to immersive journalism in regards to writing style or formatting. While immersive journalism is often narrated in first-person in the past-tense, there are no rules to how formal the writing should be or if the writing is intended for a newspaper or for a memoir. Immersive Journalism can pair with many different writing genres that will then guide these details but to qualify as immersive journalism, the text only needs to satisfy the purpose of informing through personal experience. This affords the writer plenty of space for creativity in how they develop their text in order to best entertain or inform their audience. Immersive journalism can take on the form of a video essay (like 60 Minutes) or a magazine article (DFW for Harper's Magazine) that will reach its intended audience.
TED Talks and other Multi Modes of Communication
September 24, 2017 September 25, 2017 Cameron Milne	Gateway Manis F17	Leave a comment
In searching for examples of multimodality around me, I wanted to hone in on what people don't often consider texts for the purpose of this assignment. Whether it be a financial spreadsheet or a grocery store receipt, we often overlook how those texts are formatted visually, spatially, linguistically and aurally or gesturally if presented that way. Over the last few days, I noticed a few examples of texts that requested further understanding into why the elements of that texts are arranged as such. In this assignment, I contrast the the grocery store receipt and the romantic comedy, compare the vintage circus sign and the modern billboard advertisement, and discuss why Ted Talks are effective.
The Grocery Store Receipt vs. Romantic Comedy
Date noticed: Sept. 22, 2017
These two are examples of texts that are vastly different in rhetorical situation. The grocery store receipt is a series of tightly arranged lines containing an item and a price. The linguistic goals are to inform the grocery shopper of factual information of what was purchase. Aural and gestural modes of communication are absent. Visually, a receipt is just black text overlaid on a narrow white strip of thin paper. It relies heavily on the linguistic mode to serve the purpose of its existence. Spatially, it is not designed for the shopper to marvel at it's beauty but rather to save paper thus the tightly spaced lines. In contrast, the romantic comedy movie serves an entirely different rhetorical situation and thus differs in audience, situation, and purpose. The romantic comedy, or rom-com, comes through the visual format to tell a story about two people who are somehow emotionally attached. Within the film, the blocking of the characters composes the spatial element of that format. The audience reacts to certain scenes and shots based on the characters gestures among other elements. The script, the words spoken by actors, comprises the linguistic mode of communication. Aural and gestural modes are conveyed through the acting, which attempts to mimic realism. Therefore, the two texts are different in nearly every characteristic of their existence.
Vintage Cotton Candy Sign and the Modern Fanta Billboard Advertisement
Date thought of: Sept. 23, 2017
After watching a tv show (American Horror Story; Freak Show), I noticed the font of a vintage circus sign and found myself comparing it to a modern billboard sign. Both texts had similar rhetorical situations: an image of a product with visually appealing colors and design with the purpose of attracting and maybe informing customers of that food/beverage product. Both offer visually and spatially pleasing information to look at; the colors, the arrangement of the imagery relative to the framing. The visual mode is the appropriate approach when trying to sell a product to consumers and these signs attempt to entice customers through attractive imagery lacking the linguistic mode. Both images are not filled with information, they are meant to be simple to look at with a hope of planting the thought of that product in the consumer's mind.
Date realized: Sept. 24th, 2017
I was able to find one example of a 'text' that use all five modes of communication (linguistic, aural, visual, spatial, gestural). The TED, as it was called in its first appearance in 1984, began as an event where the two founders could demo items such as the compact disc and 3D graphics for an audience. The brand lost money and failed to excite audiences until they began to use other members to share their stories. Attracting speakers that were scientists, philosophers, musicians, business leaders, and more became an effective way to capture the attention of curious, open-minded audiences. The company officially became a non-profit organization in 2001 designing the brand that we see today in 2017: seeking the most interesting people on Earth and letting them communicate their passion.
Over the last fifteen years, what had transformed into TED Talks had accumulated interest and had become an established platform for interesting people to share ideas worth spreading. If you were a psychologist with something that needed to be publicly known, your goal was to become a TED speaker. Even today, it's easy to get swept away with the over 1400 existing TED talks one can find on the internet. But what makes their videos so effective in capturing audiences and delivering important messages?
The purpose of TED Talks are to share ideas worth spreading, yet when looking closer at the structure of their presentations, they utilize each of the communication modes to entertain their audience as much as possible. Aside from the speakers use relatable topics such as happiness, knowledge, ethics, food, or psychology, they tap into the best qualities of every form of communication to deliver the most enjoyable experience possible.
The first mode of communication utilized is the visual mode. By pairing the speakers words with visual depictions of the content, they are strengthening their argument and drawing focus to something interesting outside of their own voice. Rather than just say Mickey Mantle was the best Yankees baseball player, they will show a picture in tandem to give a face to the name. There is small gray area where visual information adds value to a presentation rather than distracting, confusing, or even irritating the audience. The the slide decks are clean and empty of any words that would require the viewer to deter their attention from the speaker. Yet the pictures also effectively complement the speaker's words to enhance the viewer's experience. The successful TED speaker maximizes the benefits of visual storytelling to improve their own presentation.
The speakers also employ aural channels of communication to create an interesting dialogue that maintains the audience's curiosity throughout the talk. Captivating speakers employ verbal patterns, strategies and rhetoric that are intended to be effective. By fluctuating their voice tone, volume and pitch, their incorporating variety into their presentation that is far more enjoyable than monotonous fact reporting. They put emphasis on certain words that attune the audience to the message they are communicating. We can infer the speakers are not reading off scripts or memorizing their lines from their conversational approach..
Even the titles of their presentation impact whether viewers will choose to listen. Personally, I would sooner click on a video titled "How Great Leaders Inspire Action" (Simon Sinek) over a presentation titled "Learning from Leadership's Missing Manual" (Fields Wicker-Miurin). The linguistic techniques used by speakers matter immensely. Word choices is all too important in these videos as they tend to be the first impression on a viewer in those first ten seconds. The successful speakers are forward with their content, making short but intriguing claims such as "On a given day, studies show that you may be lied to anywhere from 10 to 200 times" (How to Spot a Liar, Pamela Meyer) before diving into an explanation. At a TED Conference, the speaker has only eighteen minutes to share their story. Therefore, any moment they spend validating a claim is wasted time and will bore the audience. Linguistic choices made by speakers have the power to enrapture an audience or lull it to sleep.
The reason viewers watch TED Talks rather than just read about the findings of a study or theory online is because of the public speaking element. Each of the speakers convey a stage presence that's noticeably charismatic. They use their hands in a way that opens the audience to trusting them. And it is the use of these nonverbal communication techniques that drive the success of TED Talks. Unlike your high school public speaking class, nobody is pacing or making untimely, awkward gestures. TED speakers speak to everyone in the audience with eye contact that sweeps the entire audience. Often, they smile to communicate confidence and intelligence. Their gestures are warm, displaying approachability, and openness. Never has there been a successful, motivational speaker that has had poor posture or arms folded at the chest. They utilize specific to gestures that assist in their ethos and pathos. And we as the audience subconsciously open up to a speaker that gestures to their openness.
TED talks also utilize the spatial mode of communicating in a unique way that written texts cannot compare. Through video editing, TED manipulates the way audiences view the speakers and their presentations. In any given TED Talk on the internet, the viewer will notice that it's not just one long take of someone speaking. The video interchanges between various camera angles, jumping from the speaker to a shot of their powerpoint. Dramatic points are further enhanced through close up shots of their face. Moments of explanation are sometimes paired with a shot that pans over the audience. The constant variety of how we view the TED Talk is an example of how their utilizing spatial modes of communicating their presentations.
Because of the way TED has been able to engage their audiences in every available form of communication, they have risen to the pinnacle of public speaking, idea sharing, and unique storytelling.

redpajama_set_name: RedPajamaCommonCrawl


BETH POLLOCK lives in Toronto, Ontario. She has written three books in the Streetlights series. Her Streetlights novel The Next Step was chosen as a Resource Links Year's Best in 2009 and The Witch of Bloor Street was chosen as a Resource Links Year's Best in 2011.
Eleven-year-old Harley doesn't ask for much. After all, her young mother works hard to make ends meet. How can she complain when so many people in their neighbourhood are worse off? But Harley has a secret wish for Mom and Grandma to settle their differences before Christmas.


My sweet Batesville friends gave us the most fun baby shower and the sweetest Walter Anderson print for the baby room(pictured behind me and the hostesses)! We got so many wonderful gifts and had such a fun time with our very close friends. (Pictured: Amanda Dawkins Overton, Stephanie Guckert, Meredith Carlson Flemming, me, Lindsey Rice Petit, Megan Dawkins(soon to be Aldridge), and Amy Rivers.
Love the painting! It will look great in your nursery!


A version of this article appeared in the print edition of The Daily Star on February 27, 2018, on page 9.
The outgoing U.N. human rights chief Monday accused the veto-wielding members of the U.N. Security Council of being second only to criminals who kill and maim when it comes to responsibility for some of the world's most egregious rights violations. Zeid Ra'ad al-Hussein delivered one of the strongest and clearest denunciations yet from a top U.N. official about certain uses of the Security Council veto, which gives extraordinary powers to the five countries that wield it: Britain, China, France, Russia and the U.S.
Speaking to the Human Rights Council, Hussein didn't mention specific vetoes.


text:
\subsection{Spectroastrometry.}
``Differential Speckle Interferometry" as the progenitor of the spectroastrometry was
first suggested by J. M. Becker\cite{Becker1982} and its feasibility was demonstrated
by R. Petrov\cite{Petrov1992}. We follow the description of interferometry in Ref.\cite{Petrov1989}
(but see also Ref.\cite{Rakshit2015} for more extensive discussions). Spectroastrometry
is a powerful tool of high spatial resolution. Given the surface brightness distribution
of the regions, we have
\begin{equation}\label{eq:ph-center}
\bm{\epsilon}(\lambda) =
\frac{\int \bm{\alpha} {\cal O}(\bm{\alpha},\lambda)  \dd[2]{\bm{\alpha}}}
{\int {\cal O}(\bm{\alpha},\lambda) \dd[2]{\bm{\alpha}}},
\end{equation}
where ${\cal O}(\bm{\alpha},\lambda)={\cal O}_{\ell}+{\cal O}_{\rm c}$ is the surface brightness
distribution of the source contributed by the BLR and continuum regions, respectively, and
$\bm{\alpha}$ is the angular displacement on the celestial sphere. Given the geometry and
kinematics of a BLR, its ${\cal O}_{\ell}$ can be calculated for one broad emission line
with the observed central wavelength $\lambda_{\rm cen}$ through
\begin{equation}\label{eq:calO}
{\cal O}_{\ell}=\int \frac{\Xi_r F_{\rm c}}{4 \pi r^2} f(\bm{r},\bm{V})
\delta\!\left(\bm{\alpha}-\bm{\alpha}' \right)
          \delta\!\left(\lambda -\lambda^{\prime}\right)
         \dd[3]{\bm{r}} \dd[3]{\bm{V}},
\end{equation}
where $\lambda^{\prime}=\lambda_{\rm cen}\gamma_{0}\left(1+\bm{V}\vdot\bm{n}_{\rm obs}/c\right)
\left(1-R_{\rm S}/r\right)^{-1/2}$ includes gravitational shifts due to the central
black hole, $\gamma_{0}=\left(1-V^2/c^2\right)^{-1/2}$ is the Lorentz factor,
${\bm \alpha}^{\prime}=\left[\bm{r}-\left(\bm{r}\vdot\bm{n}_{\rm obs}\right)\bm{n}_{\rm obs}\right]/D_{\rm A}$,
$\bm{r}$ is the displacement to the central BH, $\Xi_r$ is the reprocessing coefficient
at position $\bm{r}$, $f(\bm{r},\bm{V})$ is the velocity distribution of the clouds
at that point, $F_{\rm c}$ is ionizing fluxes received by an observer, and
$\bm{n}_{\rm obs}=(0,\sin i_{0},\cos i_{0})$
 is the unit vector pointing from the observer to the source.
Introducing the fraction of the emission line to total ($\ell_{\!\lambda}$), we have
\begin{equation}\label{eq:epsilon}
\bm{\epsilon}(\lambda) = \ell_{\!\lambda}\,\bm{\epsilon}_{\ell}(\lambda),
\end{equation}
where
\begin{equation}
\bm{\epsilon}_{\ell}(\lambda) = \frac{\int \bm{r} {\cal O}_{\ell}
   \dd[2]{\bm{\alpha}}}{\int {\cal O}_{\ell} \dd[2]{\bm{\alpha}}},\,\,\,\ell_{\!\lambda}
= \frac{F_{\ell}(\lambda)}{F_{\rm tot}(\lambda)},\, \ \ F_{\ell}(\lambda)
= \int {\cal O}_{\ell} \dd[2]{\bm{\alpha}}, \ \
   F_{\rm tot}(\lambda)=F_{\ell}(\lambda) + F_{\rm c}(\lambda). \nonumber
\end{equation}
Inserting Equations (\ref{eq:epsilon}), (\ref{eq:calO}) and (\ref{eq:ph-center}) into (\ref{eq:phase}),
we can obtain phase curves.
Since $\bm{B}/\lambda\sim 100{\rm m}/2.2\mu{\rm m}$ and $\bm{\epsilon}\sim 100{\mu\rm as}$,
$\phi_{*}$-amplitudes are expected to be at a level of a few degrees for spatial resolution
of compact objects. If the BLR model is specified, the spectroastrometric technique is able to
efficiently improve the spatial resolution.

\subsection{Reverberation mapping.}
AGNs and quasars are radiating with huge power and their spectra are prominently characterized
by broad emission lines from NIR, optical to ultraviolet
bands\cite{Osterbrock1986,Osterbrock1989,Ho2008}.
The standard model of AGNs is accretion onto supermassive black holes (SMBHs) located in galactic
centers producing powerful radiation\cite{Rees1984}. Emission lines from the photoionized gas
are broadened by fast motions under the gravitational potential of the SMBHs and appear with a
full width at half maximum (FWHM) spanning from $\sim 10^{3}$ to a few $10^{4}\rm km\,s^{-1}$. According to
energy conservation, the covering factor of the BLR clouds is about 10\%, representing a fraction
of reprocessing energy released by the accretion. As a natural consequence of
photoionization, the emission lines will follow variations of the continuum, but with a
delay denoted as $\tau_{\rm BLR}$. This delayed response is known as the reverberation
of the BLR\cite{Peterson1993}. Considering that the recombination timescale
$\tau_{\rm rec}\approx (n_{e}\alpha_{\rm B})^{-1}\approx 0.1\,n_{10}^{-1}\,$\,hr is much
shorter than $\tau_{\rm BLR}$, the delays of the emission lines represent the linear
dimension of the emission line regions, where $n_{10}=n_{e}/10^{10}{\rm cm^{-3}}$ is
electron density of clouds and $\alpha_{\rm B}$ is the case B recombination
coefficient\cite{Osterbrock1989}.

RM observations measure the LCs of
broad emission lines and continuum, and then allow us to investigate the temporal relation between
the lines and the continuum for the BLR geometry and kinematics\cite{Peterson1993}.
Echo of emission lines to the continuum was suggested earlier\cite{Bahcall1972}, but observation
campaigns began to measure it since 1980s. Nowadays, RM technique is regarded as the most powerful
tool of measuring the central black hole mass\cite{Peterson2014a} in studies of the so-called
coevolution of SMBHs and galaxies\cite{Ferrarese2005}. There are $\sim$ 100 AGNs with robust
H$\beta$ RM measurements (summarized in Ref.\cite{Kaspi2017}), this number is expected to
dramatically increase contributed by several RM groups over the word in near future.
In practice, $\tau_{\rm BLR}$ can be easily measured from the simple cross-correlation
function, however, its exact meaning can only be specified through modeling the BLR.

\subsection{Parameterized BLR.}
The understanding of BLRs has been advanced much after great efforts of RM campaigns for about
100 AGNs during the last several decades\cite{Peterson1998,Kaspi2000,Bentz2013,Du2018}.
It has been found that, except for optical Fe\,{\sc ii}-strong AGNs\cite{Du2018,Du2019}, BLR sizes
follow a well-established $R-L$
relation\cite{Bentz2013,Du2018} agreeing with the consequence of photoionization of isotropic
ionizing sources. These Fe\,{\sc ii}-strong AGNs\cite{Du2018} are mostly super-Eddington objects powered
by slim accretion discs\cite{Abramowicz1988,Wang2014b, Wang2014a}, breaking the assumption of
isotropic ionizing sources made in the explanation of H$\beta$ line reverberation\cite{Wang2014a}.
Self-shadowing effects due to the puffed-up inner part of slim disks greatly obscure illuminations
of the BLR so that H$\beta$ lags are significantly shortened\cite{Wang2014a,Du2018}.
For Fe\,{\sc ii}-weak AGNs, they are likely powered by geometrically thin accretion discs and can be well
approximated as isotropic sources. Secondly, a disc-like BLR has been generally
found in many broad-line Seyfert 1 galaxies from velocity-resolved delay
maps\cite{Grier2013,Bentz2013,Lu2016,Du2016b,Xiao2018}, even in some narrow-line Seyfert
1 galaxies\cite{Du2016b}. Moreover, the differential phase curves of the Pa$\alpha$
line in 3C 273 directly show evidence for a Keplerian rotation of flattened
disc as the BLR. Third, there is growing evidence
for Keplerian rotation of the BLR clouds through multiple campaigns of several AGNs, such
as, NGC 5548, NGC 3783, 3C 390.3 and NGC 7469\cite{Peterson2004}, stratified
radial structure of the BLR according to the ionization energy of ions in
NGC 5548\cite{Peterson2000}, or vertical structure of the
BLR (see Figure\,24 in Ref.\cite{Kollatschny2014}). Additionally, the angle between the
direction of orbital angular momentum and the $Z$-axis is uniformly distributed
over [0, $\theta_{\rm opn}$], which is used in BLR modeling\cite{Sturm2018}.
As the zero-order approximation of the present scheme, we simply assume that the BLR
clouds are orbiting with Keplerian velocity around the central black hole in this paper.
In such a characterized BLR, emission line profiles are usually symmetric.
See Supplementary Figure 1 for the BLR geometry.

With the goal of illustrating a new scheme to determine distances, we employ a stream
lined model of the BLR, rather than a comprehensive BLR model
(with about $\sim 20$ parameters) pursuing fine fitting of the observational data
as done in Ref.\cite{Pancoast2011,Pancoast2014,Li2013,Li2018,Williams2018}.
The BLR model could include more components in the future if GRAVITY data is significantly
improved.

We point out that the ``clouds'' used in this paper can be generally understood
as elements of the BLR if it is a kind of fluid. These clouds could be supplied by the
central black hole tidal capture of clumps from torus\cite{Wang2017} or winds from accretion
disc\cite{Czerny2011}. The former model keeps a quasi-stationary state of the BLR whereas some
clouds switch to the accretion disc of the black hole.

\subsection{RM$^{\rm 1D}$ modeling.}
Detailed descriptions of RM$^{\rm 1D}$ modeling of the BLR are given by Ref.\cite{Li2013,Li2018}.
Here we briefly summarize the necessary formulations for the reader's convenience. In order to
interpolate and extrapolate the sampled LC of the varying continuum, we use the damped random
walk (DRW) model to describe the continuum variations\cite{Kelly2009,Zu2013}. For a time series
of $\bm{y}$, the measured data can be expressed by
$\bm{y}=\bm{s}+\bm{n}+\bm{E} q$,
where $\bm{s}$ is the variation signal that is described by the DRW model, $\bm{n}$ is the
measurement errors, $q$ is the mean values of the series, and $\bm{E}$ is a vector with all
unity elements. The covariance function of the DRW model is given by
\begin{equation}\label{eq:S}
S(t_1,t_2)=\sigma_{\rm d}^{2}\exp\left(-\frac{|t_{1}-t_{2}|}{\tau_{\rm d}}\right),
\end{equation}
for any two points at times $t_{1}$ and $t_{2}$, where $\sigma_{\rm d}$ is the long-term standard
deviation of the variations and $\tau_{\rm d}$ is the typical timescale of the
variations\cite{Kelly2009}. Supposing that both $\bm{s}$ and $\bm{n}$ are Gaussian and
unrelated\cite{Li2013,Li2018}, the best estimate of $q$ is given by
\begin{equation}
\hat{q}=\frac{\bm{E}^{T}\bm{C}^{-1}\bm{y}}{\bm{E}^{T}\bm{C}^{-1}\bm{E}},
\end{equation}
where the superscript ``{\it T}\,'' denotes the transposition, $\bm{C}=\bm{S}+\bm{N}$, $\bm{S}$
and $\bm{N}$ are the covariance matrix of the signal $\bm{s}$ and noise. Using Bayes' theorem,
we can recover the damped random walk process to determine the best values of $\sigma_{\rm d}$ and
$\tau_{\rm d}$ for a given set of the series. The most probable estimate of the variation signal
$\bm{s}$ at any time $t_{\star}$ is given by
\begin{equation}
\hat{\bm{s}}=\bm{S}^{T}\bm{C}^{-1}(\bm{y}-\bm{E}\hat{q}).
\end{equation}
A typical realization for the continuum LC is\cite{Li2018}
\begin{equation}\label{eq:fc}
f_{\rm c} = {({\boldsymbol u}_s + \hat\bm{s})} + \bm{E}(u_q-\hat q),
\end{equation}
where ${\boldsymbol u}_s$ follows a Gaussian  process with a zero mean and covariance of
${\boldsymbol Q}=[\bm{S}^{-1}+\bm{N}^{-1}]^{-1}$, and $u_q$ follows a Gaussian process with
a zero mean and covariance of $(\bm{E}^{T}\bm{C}^{-1}\bm{E})^{-1}$. We treat ${\boldsymbol u}_s$
and $u_q$ as free parameters, which are further constrained by the LC data of the emission
line.

All calculations are done using the coordinates shown in Supplementary Figure 1.
Given the BLR geometry and kinematics, we can calculate the
response of the entire BLR to the varying continuum in order to fit the observed data.
The time-dependent fluxes of the broad emission line can be calculated by summing up
the reprocessing emissions from all the BLR clouds as
\begin{equation}\label{eq:fl}
f_{\ell}(t)=\int\dd{\bm{r}}\dd{t^{\prime}}\frac{\Xi_{r}f_{\rm c}(t^{\prime})}{4\pi r^{2}}n(\bm{r})
\delta\left(t^{\prime}-t+\tau\right)
\end{equation}
where $\tau = (r - \bm{r}\vdot\bm{n}_{\rm obs})/c$, $\Xi_{r}$ is the reprocessing
coefficient and $n(\bm{r})$ is the number density of the clouds. Given the BLR model,
Equations (\ref{eq:fc},\ref{eq:fl}) are used to fit the observed LCs denoted as
the RM$^{\rm 1D}$ analysis.

\subsection{Observational data and de-trending.}
We note that the varying continuum has a long decreasing trend, but H$\beta$
LC does not have the same trend\cite{Zhang2019} (also see Supplementary
Figures 4 and 5).
It has been suggested
that de-trending is an efficient way to improve the RM analysis of long-term
secular variability of continuum\cite{Welsh1999,Peterson2004}. In the present scheme
of fittings, we take a linear form of de-trending as $f_{\rm c}\propto k_{\rm c}(t-t_{0})$
for the continuum LCs, where $k_{\rm c}$ is determined by the joint analysis.

\subsection{\it Contamination.}
In Supplementary Figure 4,
we show the $\gamma$-ray LC monitored by the LAT of the
{\it Fermi} satellite (https://fermi.gsfc.nasa.gov/ssc/data/access/). The
$\ge 30$GeV emission must be generated by the most inner part of the jet\cite{Blandford1995},
and thus contamination could be tested by $\gamma$-rays. The {\it Fermi} monitoring campaign
is continuous without season gaps, allowing us to test the long-term trend. We generate the
$\gamma$-ray LC according to the {\it Fermi} user's Guider (see also the $\gamma$-ray
LC in Ref.\cite{Meyer2019}). It is obvious that there is a giant $\gamma$-ray flare in the second
half year of 2009 and first months of 2010, and the flare has a long tail lasting to the
end of 2011. It is not the goal of the present paper to make a detailed comparison between the
$\gamma$-ray and $V$-band LCs, but it is quite obvious that the flare significantly contributes
to the observed optical continuum. It is also clear that the response of the broad H$\beta$
line to the optical continuum is weak. The jet contamination has been investigated\cite{Li2019}
through analysis of multiple long-term light curves from radio to optical band, as well as
polarization. It is clear that the long term trend of 5100\AA\, continuum is due to the jet
contaminations. See details in this reference.

\subsection{\it Weak response of the broad H$\beta$ line.}
Entire LCs are shown by Supplementary Figure 5{\it a}, 5{\it b} and 5{\it c}.
With the de-trended continuum LC, we obtained a lag of
$\tau_{\rm BLR}=146\pm 8$\,days\cite{Zhang2019}.  We shifted the H$\beta$ LC backward by the
$(1+z)\tau_{\rm BLR}$ and multiplied $F_{\rm H\beta}$ by a reasonable factor for a compare
with the de-trended continuum in Supplementary Figure\, 5{\it d}.
It is clear that the response of H$\beta$ is weak before 2012. One plausible reason is that
the optical continuum is contaminated (UV is less significantly) by the jet located
outside the BLR, but the BLR has no response to this continuum component. We only focus
on the linear response at the zero-order of the model, rather than non-linear responses
of the BLR clouds in this paper.

\subsection{Fittings.}
Clouds are randomized to distribute along a given orbit. We use this prescription
of cloud distribution for the calculation of transfer functions, line profiles, and
differential phase curves. Special and general relativistic effects are included.
We take the priors of the BLR parameters in sufficiently wide ranges in order to
guarantee the unique solutions of the model. Ranges of parameters are provided in
Table 1. The priors of
$(\mathscr{F},\beta,\theta_{\rm opn},i_0,{\rm PA})$ are uniform over the given
intervals, while those of $(R_{\rm BLR},M_{\bullet},D_{\rm A})$ are uniform in
log scale. The cosmological dilation factor of $(1+z)$ has been included in generating
LC to fit observations of 3C 273 in the BLR modeling. Using the Diffusive Nested
Sampling\cite{Brewer2018}, we obtain a total of $5000$
samples for all model parameters.
We generate probabilities in Equation (\ref{eq:probability}), $P^{f_{\ell}}_{i}$
for H$\beta$ reverberation, $P_{i,j}^{\phi}$ for differential phase curves and
$P_{j}^{F_{\ell}}$ for profiles of the Pa$\alpha$ line,
\begin{equation}
P^{f_{\ell}}_{i}=\frac{1}{\sqrt{2 \pi\sigma_{\ell}^{2}}}
\exp \left\{-\frac{\left[f_{\ell,i}^{\rm obs}-f_{\ell,i}^{\rm mod}\left(f_{\rm c, obs} |
\bm{\Theta}\right)\right]^{2}}{2\sigma_{\ell}^{2}}\right\},
\end{equation}

\begin{equation}
P_{i,j}^{\phi}=\frac{1}{\sqrt{2 \pi \sigma_{\phi_{ij}}^{2}}}
\exp \left\{-\frac{\left[\phi_{i,j}^{\rm obs}-\phi_{i,j}^{\rm mod}
\left(\bm{\Theta}\right)\right]^{2}}{2\sigma_{\phi_{ij}}^{2}}\right\},
\end{equation}

\begin{equation}
P_{j}^{F_{\ell}}=\frac{1}{\sqrt{2 \pi \sigma_{\rm F}^{2}}}
\exp \left\{- \frac{\left[F_{\ell,j}^{\rm obs} - F_{\ell,j}^{\rm mod}\left(\bm{\Theta}\right)\right]^{2}}
{2\sigma_{\rm F}^{2}}\right\},
\end{equation}
where $f_{\ell,i}^{\rm obs}$, $F_{\ell, j}^{\rm obs}$, and $\phi_{i,j}^{\rm obs}$ are the
observed line flux, line profile, and interferometric phase of the emission line with
measurement uncertainties $\sigma_{\ell}$, $\sigma_{\phi_{ij}}$, and $\sigma_{\rm F}$,
respectively, and $(f_{\ell,i}^{\rm mod},F_{\ell,j}^{\rm mod},\phi_{\ell,i}^{\rm mod})$
are the corresponding predicted values from the BLR model.

The joint analysis of the SARM data shows the reduced $\chi^{2}_{\rm G}=1.33$ for GRAVITY data
and $\chi^{2}_{\rm RM}=1.61$ for the RM data. The $\chi^{2}_{\rm RM}$ is a little bit higher
than $\chi^{2}_{\rm G}$, but note that this could be caused by a couple of points in the H$\beta$
LC significantly deviating from the model. Excluding these points, we find that the $\chi^{2}$ will
be greatly reduced. Considering the major goals of the present paper, we keep this fitting
with the $\chi^{2}=1.61$ as resultant fittings. We found $k_{\rm c}=(7.9\pm 0.2)\times 10^{-5}$
from the joint fitting, which is consistent with the results in Ref.\cite{Li2019}

We generated mock data to test the present scheme. Error bars of GRAVITY phase curves are
set to be $\sim 25\%$ and RM data at the level of the 3C 273 campaign. We find that the
generated parameters of the model from the mock data are in good agreement with the input
within 10\%. This demonstrates that the present joint analysis is feasible for simultaneous
determinations of distances and black hole mass of AGNs.

\subsection{Quasars as cosmological probes.}
Quasars are the most luminous and long-lived celestial objects in the Universe. After their
discovery, they were instantly suggested as probes for
cosmology\cite{Sandage1965,Hoyle1966,Longair1967,Baldwin1977} by arguing that some properties
of quasars can serve as ``standards''. However, these efforts were
not successful because of poor understanding of quasar physics. Recently, interests in
applications of quasars to cosmology have arisen again by selecting special individual
objects or populations in light of their well-understood properties.

Direct measurements of distances through very long base interferometry (VLBI) observations of
water masers in NGC 4258 ($z\approx 0.0015$)\cite{Humphreys2013}, and torus diameters through
direct imaging observations of NGC 4151 ($z\approx 0.0033$)\cite{Honig2014} have been suggested
for cosmology,
but these methods are limited either by the rare sources of water masers or the long period of
NIR monitoring campaigns. Parallax of quasar BLR was suggested for measurements of
distances\cite{Elvis2002,Quercellini2009},
which needs an interferometer with a baseline of $\sim 100$km, but GRAVITY at The Very Large Telescope
Interferometer (with baselines of only $\sim 100$m) employs spectroastrometry to efficiently reduce
the required baseline for 10$\mu$as resolution. Super-Eddington accreting massive black holes
(SEAMBHs over much wider ranges of redshifts) from their saturated
luminosity\cite{Abramowicz1988,Wang1999,Wang2013,Du2014,Wang2014a,Marziani2014,Du2018} were suggested
for cosmology and show potential feasibilities of application to the high-$z$ Universe\cite{Cai2018}.
Moreover, the following relations have been also suggested for cosmology, such as the
well-known $R-L$ relation of sub-Eddington AGNs\cite{Watson2011,Czerny2013,King2015} or
its improved version\cite{Martinez2019}, NIR continuum reverberation correlation\cite{Yoshii2014},
X-ray variance versus luminosity\cite{LaFranca2014}, and the non-linear UV versus X-ray
luminosity relation\cite{Risaliti2019}. Quasars as cosmological
objects seem to be a promising tool to probe the Universe in future\cite{Czerny2018,Marziani2019},
but much work needs to be done for precision cosmology as a robust probe.

We would like to point out that all the methods mentioned above need calibrations of cosmic
ladders except for the way of the VLBI water maser and NIR RM techniques.
The application of the $R-L$ relation to cosmology has been
initiated\cite{King2015,Czerny2019,Hoormann2019}, but emission-line lags for high-$z$ quasars
are hard to measure because of the dilation factor of $(1+z)$. SEAMBHs as a new
kind of cosmic ladders can be in principle extended to high-$z$
quasars\cite{Negrete2018,Martinez2018} from the local scaling relation\cite{Du2016a}.

Moreover, the present SARM analysis provides a direct method without the calibration issues
of known cosmic ladders or extinction corrections.
Future GRAVITY observations of low-$z$ SEAMBHs will provide an efficient way of calibrating
SEAMBHs into the high-$z$ Universe. It is then expected to use AGNs for accurate measurements
of distances from low-$z$ to high-$z$ Universe. Calibrations by different ladders are not
necessary in the current approach.

As inquired by one of referees, we applied the simplest estimation of 3C 273 distances
through torus image and NIR RM data.
The angular size of its torus is $\Delta \theta_{\rm tor}=0.29\,$mas is from Keck interferometer
observations\cite{Kishimoto2011} and the linear size $\Delta R_{\rm tor}\approx 1.0\,$lt-yr from
the long term $K$-band light curve and the optical-UV\cite{Soldi2008}. We have a distance of
$D_{\rm A}=\Delta R_{\rm tor}/\Delta\theta_{\rm tor}\approx 212\,$Mpc, which is smaller
a factor of 2.6 than the present determination and the $\Lambda$CDM model, but it is still
encouraging. We note that the $K$-band light curve has too poor cadences after 1995 to reliably
determine $\Delta R_{\rm tor}$ (see their Figure 2 in Ref.\cite{Soldi2008}),
moreover, this estimation needs to be improved through the sophisticated scheme to obtain
$\Delta R_{\rm tor}$ and $\Delta\theta_{\rm tor}$ for distances like in Ref.\cite{Honig2014}.
It should be noted that NIR continuum RM campaigns are usually much longer than the H$\beta$
ones.

\subsection{Uncertainties from the BLR model.}
Geometrical measurements of both GRAVITY and the RM data depend on the BLR model, which is assumed
to be a geometrically thick disc with Keplerian rotation. More complicated structures and kinematics
of the BLRs are possible, however, we should note that they can be observationally tested for
systematic errors, which can be independently estimated from observational data
of RM campaigns through comparing with mock data.

\subsection{\it Differences compared with sole GRAVITY measurements.}
As shown in Table 1 and Supplementary Figure\, 3,
some results from the SARM analysis are significantly different from that from analysis of
sole GRAVITY data, however they seem to be reasonable. As shown by Equation (\ref{eq:phase}),
the phase curves are more sensitive to the BLR information projected
to the baseline direction. RM of broad H$\beta$ line mainly delivers its information along LOS.
With different sensitivities of GRAVITY and RM data on model parameters,

the joint analysis gets benefits from that some degeneracies of parameters are
broken by the simultaneous application of both databases} and
hence generates more robust results. For example, the SARM analysis
yields $M_{\bullet}=5.78_{-0.88}^{+1.11}\times 10^{8}M_{\odot}$ with relative errors smaller than that
of $M_{\bullet}=2.6\pm 1.1\times 10^{8}M_{\odot}$ from the pure SA analysis\cite{Sturm2018} (we noted
a $\sim 2.0\sigma$ $M_{\bullet}$-tension here).
The SARM-measured $M_{\bullet}$ is also more reliable than the simple virial mass of black hole
($M_{\rm vir}$)\cite{Zhang2019}. The reasons are obvious: $M_{\rm vir}$ depends on the virial
factor, while the factor is determined by calibrating with $M_{\bullet}-\sigma$ relation\cite{Onken2004}.
Moreover, H$\beta$ lags (even its error bars are very small) generated by cross correlation
analysis remain quite ambiguous in their exact physical meanings since the lags do not fully
cover the regions corresponding to its H$\beta$ FWHM. Currently, the lags of broad emission
lines are explained as an emissivity-averaged radius of the BLR, however,
the geometric radius can be specified after fixing a physical model. Once given
the BLR geometry and
kinematics, a joint analysis of GRAVITY and RM data generates the BLR parameters of the
best fittings for both independent datasets (GRAVITY and RM data) simultaneously.
For 3C 273, both $D_{\rm A}$ and $M_{\bullet}$ are quite robust [see the circle shapes of contours
in Supplementary Figure 3
except for $(\beta,\mathscr{F})$, $(R_{\rm BLR},\mathscr{F})$
and $(M_{\bullet},\theta_{\rm opn})$]. On the other hand, we expect SARM observations of more
targets to better understand the differences between the SARM with others (such as the slight
$M_{\bullet}$-tension).

\subsection{\it Geometry and kinematics.}
Roughly speaking, symmetric profiles of broad emission lines form from axisymmetric discs.
The characterized BLR model of a geometrically thick disc with Keplerian rotation can be
observationally tested by repeating campaigns (conveniently in principle). Velocity-resolved
delays independent of models, or the 2D delay maps obtained from maximum entropy
method\cite{Horne1991} can directly justify the BLR geometry by comparing them with the
shapes of known geometries, such as inflows or outflows\cite{Welsh1991,Xiao2018}.
Moreover, the Keplerian rotating disc follows a simple relation of
$\tau_{\rm BLR}\propto V_{\rm FWHM}^{-2}$, as in NGC 5548 and others mentioned previously.
It is thus feasible to estimate the uncertainties
of BLR geometry and kinematics contributed to systematic error bars of the model parameters.

We should note that GRAVITY measured the Pa$\alpha$ line region whereas the 10-yr RM
campaign observed the H$\beta$. A fully self-consistent scheme should employ the same line
for GRAVITY and RM campaign, however, an RM campaign of near infrared emission lines is much
harder than H$\beta$ line. As argued in the main text, we in principle expect that Pa$\alpha$
and H$\beta$ regions should be the same in the simplest model. However, $V_{\rm FWHM}$ of
H$\beta$ and Pa$\alpha$ lines are slightly different, implying the two-line regions
may mismatch due to different optical depths for H$\beta$ and Pa$\alpha$ photons. A simple
estimation can be done by following.
Supposing the averaged radius ($R_{0}$) of the BLR with a difference $\Delta R$ for the two lines,
we have $(R_{0}+\Delta R)V^{2}_{\rm Pa\alpha}=(R_{0}-\Delta R)V^{2}_{\rm H\beta}$ from
the assumption that the two-line regions are vrialized, where $V_{\rm Pa\alpha,H\beta}$ are FWHMs of
their profiles. We obtain the relative difference of $\Delta R/R_{0}=(q-1)/(q+1)$,
where $q= \left(V_{\rm H\beta}/V_{\rm Pa\alpha}\right)^{2}$. According to the long campaign of
3C 273, we have $V_{\rm H\beta}\approx (3100-3300)\rm km\,s^{-1}$ changing with luminosity\cite{Zhang2019} while
$V_{\rm Pa\alpha}\approx (2700-3000)\rm km\,s^{-1}$ from GRAVITY\cite{Sturm2018} and NASA Infrared Telescope
Facility (IRTF) observation\cite{Landt2008}. Taking the averaged values of
$V_{\rm Pa\alpha,H\beta}\approx (2800,3200)\rm km\,s^{-1}$, we have $\Delta R/R_{0}= 13\%$. This error bar
is comparable to that of distance measurements, but it can be greatly eliminated in the
RM$^{\rm 2D}$ modeling.
Additionally, statistics show that
Pa$\alpha$ line shares the same region with H$\beta$ line\cite{Landt2013}.
Ideally, RM should monitor the same emission line with GRAVITY in order to reduce the potential
differences between RM and GRAVITY detections. A NIR-RM campaign
of monitoring Pa$\alpha$ of 3C 273 is then expected for this goal.

On the other hand, the current analysis of the RM$^{\rm 1D}$+GRAVITY can be extended to
that of the RM$^{\rm 2D}$+GRAVITY through allowing for different but partially overlapped
regions for the two lines, which includes information of variations of H$\beta$
profiles in the analysis of RM data\cite{Pancoast2014,Li2018}.
In such a modeling scheme, the profile variations will be moderately sensitive
to the vertical structure of the BLR. Since
Pa$\alpha$ line share the partially same regions with the H$\beta$, we relax $\mathscr{F}$
and $R_{\rm BLR}$ to cover the two regions for different profiles of the two lines.
However, the two regions share the same geometry and kinematics,
such as, the same $\theta_{\rm opn}$ and kinematics. Moreover, parameters describing
cloud properties, such as anisotropy of line emissions, will be included in the
RM$^{\rm 2D}$ modeling\cite{Pancoast2014,Li2018,Williams2018}.
Though new parameters are added in RM$^{\rm 2D}$ modeling, there are about 300 profiles
of H$\beta$ spectra of 3C 273 available to set more constraints on the parameters,
providing opportunities to have
better measurements of black hole mass and distance. This is the major
contents of a separate paper of the joint analysis of GRAVITY and RM$^{\rm 2D}$ modeling
BLR for distances.

\subsection{\it Radiation pressure.}
Motion of BLR clouds could be affected by radiation pressure\cite{Marconi2008,Netzer2010},
which changes kinematics of the clouds. Considering that the pressure decreases with the
square of the distance to the black hole (for the simplest version of the pressure),
we can combine its effects into the gravitational
potential so that we can get the effective mass of the black hole in such a case. The effective
mass of the black hole could be slightly smaller than the present,
but the distance to observers remains the same.

Dimensionless accretion rates of AGNs can be estimated by
$\dot{\mathscr{M}}_{\bullet}=20.1\left(\ell_{44}/\cos i_{0}\right)^{3/2}M_{7}^{-2}$,
where $\dot{\mathscr{M}}_{\bullet}=\dot{M}_{\bullet}/\dot{M}_{\rm Edd}$, $\dot{M}_{\bullet}$
and $\dot{M}_{\rm Edd}=L_{\rm Edd}/c^{2}$ are accretion rates of the black hole and Eddington
rate, respectively, $L_{\rm Edd}$ is the Eddington luminosity, $\ell_{44}$
is the 5100\AA\, luminosity in units of $10^{44}\rm ergs\,s^{-1}$
and $M_{7}=M_{\bullet}/10^{7}M_{\odot}$. The $\dot{\mathscr{M}}_{\bullet}$ is derived from the
standard accretion disc model\cite{Wang2014b}. Taking $\ell_{44}=84.3$ from our RM
campaign\cite{Zhang2019} and $M_{7}=57.8$ from the SARM analysis, we have
$\dot{\mathscr{M}}_{\bullet}\approx 4.7$ in 3C 273, implying a slight super-Eddington
accretor compared with others\cite{Du2018}. In such a case, the radiation pressure on cloud's
motion is not serious for mass estimations\cite{Netzer2010}. Actually, the pressure
can be included in the joint analysis of MCM modeling for more accurate measurements of black
hole masses (or effective mass), fortunately, distance determinations escape from its influence.
We would point out that the SARM analysis provides the most accurate mass of black holes in
type I AGNs so far, and we will include radiation pressure to improve SARM analysis further
for discussions related with coevolution of SMBHs and their hosts.

\subsection{\it BLR variations.}
BLRs are known to vary with luminosities, such as in NGC 5548 (Figures 6, 8, 13 in
Ref.\cite{Peterson1999,Lu2016,Pei2017}, respectively).
Since GRAVITY observations only take a few hours, which are much shorter than durations
of RM campaigns (denoted as $\Delta t_{\rm RM}$ which is usually from a few months to years),
GRAVITY may detect the changing BLR at different epochs from the RM campaigns. This may be
one origin of the systematic uncertainties. For 3C 273, its RM
campaign is as long as 10yr whereas GRAVITY observations just took snaps
over a few hours or so in the last two years. The timescale of BLR variation is roughly
given by $\Delta t_{\rm BLR}\approx R_{\rm BLR}/V_{\rm FWHM}=42\,\tau_{150}V_{3000}^{-1}$\,yr
for dynamical changes, where $\tau_{150}=\tau_{\rm BLR}/150{\rm days}$ and
$V_{3000}=V_{\rm FWHM}/3000\rm km\,s^{-1}$. Considering $\Delta t_{\rm RM}\ll \Delta t_{\rm BLR}$,
we think that the current SARM analysis of 3C 273 avoids potential variations of the BLR
in last ten years (the ionization fronts are fast changing with luminosity as
$\Delta R_{\rm BLR}/R_{\rm BLR}\approx 0.5 \Delta L_{5100}/L_{5100}$ and it is $\lesssim 7\%$
from Supplementary Figure 5).
In order to avoid systematic errors from the BLR variations, we should do RM campaigns in the same
period of GRAVITY observations in future SARM projects. It is fortunate that GRAVITY observations
of 3C 273 was covered by our campaign, efficiently reducing this influence on the present results.

One question may be asked if the RM-measured BLR is the same with GRAVITY measured
regions because RM only measures the variable parts of the BLR and GRAVITY does the
entire. This problem can be justified by comparing the mean and the RMS spectra for differences.
For 3C 273, fortunately, it is clear that the RMS shape is very similar to its mean spectrum as shown
in Figure 2 in Ref.\cite{Zhang2019}. On the contrary, if the RMS is very distinguished  from
the mean spectra, GRAVITY measured BLR may be very different from the RM parts making the SARM analysis
elusive. In practice, GRAVITY observations can be scheduled once at the beginning and ending epochs
to find if the BLR changes. This strategy of observations can avoid the mis-matched measurements
between GRAVITY and RM.

\subsection{\it Degrees of ordered motion.}
Spectroastrometry measures the mean centers of $\lambda$-photons from the BLR and
thus depends on its angular momentum distributions, namely on the degree (${\cal{R}}_{0}$)
of ordered motion of the BLR clouds\cite{Stern2015,Rakshit2015,Songsheng2019}.
Fully ordered motion of BLR clouds, ${\cal{R}}_{0}=1$, is presumed in Ref.\cite{Sturm2018}
about GRAVITY observations of 3C 273. In
principle, ${\cal{R}}_{0}$ should be treated as a free parameter in fitting the DPCs of
GRAVITY data, but it strongly degenerates with the BLR sizes. ${\cal{R}}_{0}$ could be
estimated from the position angles of polarized spectra arising from scattering by
hot electrons in the mid-plane\cite{Smith2005,Songsheng2018}. Building up the relation
between ${\cal{R}}_{0}$ and position angles of the polarized spectra will be very
helpful to understand the ${\cal R}_{0}$ parameter of BLR clouds, but we have to
introduce more parameters describing the electron scattering zone. This is much
beyond the scope of the present paper, but we will treat this problem separately.

\subsection{\it Error budgets.}
Error sources are generally from several aspects discussed in previous sections
in additional to the measurements of GRAVITY
observations and RM campaigns (for ideal SARM observations, namely, focus on the same line).
First, the degree of disordered motion could contribute
uncertainties to the present analysis. This involves the formation of the BLR, either from
disc winds\cite{Czerny2011} or tidally captured clumps from a dusty torus\cite{Wang2017}.
We expect to test ${\cal{R}}_{0}$ through polarized spectra. Second, non-Keplerian
kinematics and a non-disc BLR could be other sources of systematic errors. Fortunately,
this can be evaluated by repeating RM campaigns of individual AGNs to demonstrate the
sources through direct test of the relation between $\tau_{\rm H\beta}-{\rm FWHM}$
and velocity-resolved delay relation ($\tau_{\rm H\beta}-V$) for the BLR geometry,
where $V$ is the velocity bin. Actually, the systematic errors can be efficiently
alleviated through selecting targets with symmetric profiles of broad emission lines.
Third, the quasi-simultaneous observations of GRAVITY and RM campaigns might
imply different regions measured by the two tools. However, this could be avoided
if the SARM observations can be performed under reasonable schedule of observations
or within a BLR dynamical timescale. Fourth, selection of radial and angular distributions
of BLR clouds in the model is another source of systematic errors for both GRAVITY and RM
data. In order to quantitatively issue the errors, we need to simulate models to show
error bars. Detailed discussions on this problem are beyond the
scope of this paper, but we leave it in a future work.

Finally, for individual 3C 273, some errors are from observations of the RM campaign.
There are a few key valleys and peaks for the
determinations of model parameters, however, they are in season gaps, such as the
second half years of 2012, 2015, 2016, 2017. Accuracies of model parameters are
then affected in the joint analysis. Actually, we continue the campaign with a goal
of getting more diagnostic valleys and peaks in next few years.

\subsection{Future SARM projects.}
Spectroastrometry and reverberation mapping must come together for excellent
studies of AGN physics and cosmology, but also for close-binaries of supermassive
black holes (CB-SMBHs)\cite{Wang2018,Songsheng2019} radiating nano-Hertz gravitational
waves (to be detected by the Pulsar Timing Arrays\cite{Burke2019}).
Only GRAVITY observations of 3C 273 have been reported so far\cite{Sturm2018},
but similar targets selected from existing catalogs are listed for future SARM project
in the Supplementary Table 1. GRAVITY will install new grisms in October 2019 so that
$K\approx 11.0-11.5$ targets can be observed as routine research of AGNs. We
note most the targets with redshifts $z\lesssim 0.08$, in which only Br$\gamma$
line (is significantly fainter than Pa$\alpha$ line) could be detected by GRAVITY.
{Simulations for 3C 120 ($K=10.78$, see Supplementary Table 1)
showed very promising detections of the Br$\gamma$ line, which was given by a talk
of M. R. Stock. It can be found from website of the workshop
({\tt https://www.torus2018.org/TALKS/18.12.10-S3.3-Stock.pdf}).
From page 15 of the talk's file, we find that Br$\gamma$ interferometric signals
are strong enough for a joint analysis in the future. On the other hand,
Br$\gamma$ line forms
from a transition of electrons from $n=7$ to 4. In such a context, we should understand
differences of Br$\gamma$ and H$\beta$ line regions through CLOUDY and  test
results from the RM$^{\rm 2D}$+GRAVITY modeling.}
 we thus expect that the
current GRAVITY observes the targets listed here in near future. Optical spectra
of all the targets are given in Supplementary Figure 6.
The targets actually cover three kinds of AGNs: 1) Fe\,{\sc ii}-strong objects; 2) candidates
of CB-SMBHs appearing with H$\beta$ asymmetry; 3) Fe\,{\sc ii}-weak objects.

A brief strategy of the future SARM projects could be as outlined below.
RM campaigns of the targets are expected to perform: 1) reveal velocity-resolved delays
for kinematics and geometry (with physical sizes); 2) construct 2-dimensional
transfer functions for justifying CB-SMBH candidates; 3) show stability of the
BLR from multiple campaigns, for the goal of establishing BLR properties including
stability of their structures.
This needs much work of 2m telescopes to prepare for GRAVITY observations. After then,
GRAVITY observations provide differential phase curves for structure, kinematics and
angular sizes of the BLR. On the other hand, RM of GRAVITY near-infrared emission
lines will, in principle, provide fully self-consistent data for the joint analysis.
In such a campaign, targets should be selected more carefully to avoid NIR absorptions
of the atmosphere. The campaigns could be conducted through 4m-class telescopes.
We outline three aspects below (but they are valid for RM campaigns of H$\beta$ line
with different broad emission lines in NIR).

SARM observations are for scientific goals as followings.
Targets will be spatially resolved by GRAVITY observations along with RM campaigns
to explore signatures of flattened rotating disc, inflows, or outflows in BLR in
order to study accretion process and formation of the BLR connecting with dusty
torus\cite{Wang2017}. In particular,
those of optical Fe\,{\sc ii}-strong AGNs (about 1/3 of PG quasars\cite{Boroson1992})
usually have smaller BLRs compared with objects with the same luminosities (significantly
downward deviating from the well-known $R-L$ relation)\cite{Du2018}, and most of them are
super-Eddington accreting massive black holes (SEAMBHs). SARM-based measurements of
SEAMBHs might reveal more details of BLR structure and kinematics as well as
physics of super-Eddington accretion process. Moreover,
super-Eddington accretion process as a key phase across cosmic time is a critical step
toward fast growth of seed black holes to form SMBHs in high-$z$
Universe\cite{Volonteri2005,Wang2006,Milo2009,Regan2019}. This is very compelling for
the increasing large samples of DESI (Dark Energy Survey Instrument) to tackle growth
and formation issues of the SMBHs. Third, SEAMBHs are suggested to be a new kind of cosmic
candles for the high-$z$ cosmology\cite{Wang2013,Wang2014b,Marziani2014}. SARM-based
measurements of SEAMBHs will build up precision ladders approaching to high-$z$ Universe.

With the unprecedented power of high-spatial resolutions, GRAVITY offers opportunity of
spatially resolve CB-SMBHs. AGNs with asymmetric profiles have likely more
complicated BLR structures, and some of them could
be CB-SMBH candidates\cite{Wang2018,Nguyen2019}.
A dedicated project of Monitoring AGNs with H$\beta$ Asymmetry (MAHA) is being conducted to
construct 2-dimensional transfer functions\cite{Wang2018,Songsheng2019a,Kovacevic2019}
through the Wyoming Infrared Observatory 2.3m telescope\cite{MAHA1} for the
CB-SMBHs of future GRAVITY observations. The MAHA project
is expected to provide the most promising candidates of the CB-SMBHs for GRAVITY, and for
a joint analysis of the SARM data\cite{Songsheng2019}. We would like to point out that
Ark 120, Mrk 704 and several others show interesting features of CB-SMBHs in their 2D transfer
functions. They are good targets of GRAVITY observations with obvious signatures of differential
phase curves\cite{Songsheng2019b} in near future. Moreover, it could
be possible to measure orbital parameters (such as masses of component black holes, inclination
and ellipticity of the orbits) by the joint analysis of SARM data
in order to predict properties of low-frequency gravitational waves radiated by the CB-SMBHs.

Optical Fe\,{\sc ii}-weak AGNs are usually sub-Eddington accretors\cite{Du2018}. We select some of them
with stable and flattened-Keplerian disc-like BLR guaranteeing physical conditions of the SARM
targets to efficiently reduce systematic errors of distance measurements of AGNs. They are
excellent targets of GRAVITY observations for cosmology outlined in this paper. Fortunately
again, this can be done by RM campaigns using 2m telescopes. From Supplementary Table 1,
we have about $N\approx (30, 50)$ targets with $K\lesssim (11.0,11.5)$, respectively. This makes
it feasible to establish a future SARM project for the $H_{0}$-measurements, providing
$\Delta H_{0}/H_{0}\lesssim (3,2)$ per cent, respectively, which are valid for a test of the
current $H_{0}$-tension. With one 4yr SRAM project for $\sim 100$ AGNs, we can achieve $\sim 1.5\%$.
If the uncertainties
($\sim\!13\%$ in 3C 273)
are included, $N\approx 200$ could be necessary. However, in principle,
this systematic errors can be alleviated by RM$^{\rm 2D}$+GRAVITY measurements, hence,
the $N\approx 200$ should be significantly reduced. On the other hand, with capability of future
interferometers in space (spatial resolution up to $\sim 1\mu$as by the {\it SIM}-Lite
for optical $\sim 20$mag AGNs\cite{Unwin2008,Ding2009}), we can accurately measure all information
of the H$\beta$ line region (angular and linear sizes) in optical bands for low-$z$ quasars so that
this systematic errors completely vanish.
The $H_{0}$-measurements can be done with unprecedented precisions by an AGN sample much smaller
than the present estimates.
GRAVITY$^{+}$ with much improved sensitivity\cite{Widmann2018} is expected
to explore high-$z$ cosmology (i.e., the Hubble parameter) through the present SARM scheme.
In this case, one needs to use larger telescope (e.g., 5m class) to monitor GRAVITY+ targets
in order to avoid too long RM campaigns. It should be stressed again that this
is geometric for high-$z$ cosmology.

In a brief summary, the near future SEAMBH-, CB-SMBH-, and $H_{0}$-SARM projects will significantly
advance understanding of AGN physics, close-binaries of supermassive black holes for nano-Hertz
gravitational waves, and precision cosmology, respectively. It is highly desired to perform
the three feasible projects in a few years.

{\bf Data Availability.} The data that support the plots within this paper and
other findings of this study are available from the corresponding author upon reasonable request.

{\bf Code Availability.} All the codes used in this paper are available from the corresponding
author upon reasonable request.

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